Interesting stuff, check it out:
http://talk.asteroidzoo.org/#/boards/BAZ0000002/discussions/DAZ0000889
The post mentions a previous Astrogator’s Guild posting:


Interesting stuff, check it out: http://talk.asteroidzoo.org/#/boards/BAZ0000002/discussions/DAZ0000889 The post mentions a previous Astrogator’s Guild posting: On CNN.com there was a story “Meteorite makes big crater in Nicaragua” by Amanda Barnett. In the article, Amanda wrote: ‘AP quoted government spokeswoman Rosario Murillo as saying they’ve determined it was a “relatively small” meteorite that “appears to have come off an asteroid that was passing close to Earth.”‘ Well, that’s enough to get someone wondering if indeed it could have come off 2014 RC, which just did the flyby this past Sunday, 7 Sep 2014 at 18:15 UTC. Well, Adam Gorski at Analytical Graphics made this easy by posting an STK scenario on AGI’s website blog: Asteroid 2014 RC flyby on Sunday. Adam got 2014 RC’s ephemeris from the JPL Horizons website, and set everything up. THANK YOU ADAM! In Amanda’s article, she says “The Nicaragua Dispatch said the hole is in the woods near Managua’s Sandino International Airport and about 1,000 feet (300 meters) from the Camino Real Hotel” which, according to Google Maps is at Latitude 12.148060, Longitude 86.184949. So, I put this into STK as a place object. Amanda also mentions the time of impact, which is critical to this: “The Today Nicaragua site reported the crater was found after a loud blast about 11:05 p.m. on Saturday. ” Nicaragua is in the Central Time Zone, and from a few web searches seems that they do not use daylight savings time. So the time should be UTC – 6 hours. So, 11:05 pm on Saturday would be 7 Sep 2014 05:05 UTC. So, with the location and the time, we can see if the Hotel was on the side of the Earth from which the asteroid was coming from: So, that seems pretty obvious. (Even if the time is off by an hour or so, it’s still on the correct side of Earth.) In this STK view, asteroid 2014 RC is traveling from lefttoright, and the hotel near which the crater was found is on the same side of the Earth. So far this myth is NOT busted; it’s plausible. So the direction seems reasonable, but we want to see if it’s reasonable that this meteorite could have come off of asteroid 2014 RC. We can use a similar approach that several us did a few years ago investigating a potential space debris collision, as written in the paper “INVESTIGATING ORBITAL DEBRIS EVENTS USING NUMERICAL METHODS WITH FULL FORCE MODEL ORBIT PROPAGATION.” (by Timothy Carrico, John Carrico, Lisa Policastri, Mike Loucks, AAS 08126.) We can see if a reasonable force applied in the past could have knocked a rock off of 2014 RC, or perhaps another impact caused a chunk to be thrown off. We can model this in STK/Astrogator by getting an initial state for 2014 RC in the past, and calculate what deltaV (change in velocity) would be needed to divert from 2014 RC’s trajectory to hit near the hotel at the observed time. Not knowing when the meteorite could have left its host, I chose to investigate the case if the rock left the asteroid 10 years ago. So, using our favorite “Follow Segment” in Astrogator, I propagated the initial state of the Asteroid that Adam had found backwards in time for ten years. Then I modeled a small impulsive deltaV, and set up the Astrogator targeter to calculate the deltaV needed to hit the hotel at the specific time. I set up the targeter to hit Earth BPlane values of B dot T = 0.0, and B dot R = 0.0 (hitting the Earth right in the middle, as seen from the approaching asteroid). And when that profile converged, the next targeting profile targeted the exact latitude and longitude of the hotel. This converged pretty quickly, and gave a deltaV number of about 90 meters/second. Since an impact velocity of an asteroid could be 10 or more km/second, this low value seemed very reasonable. And, if the rock had come off a hundred, or several thousand years ago, it would take even less deltaV to hit near the hotel. So, once again, the myth is NOT busted, and it’s very plausible that this meteorite came off of asteroid 2014 RC as some point in the past.
Astrogator John The Chang’e 3 Lander is on the surface! What an amazing accomplishment for our Chinese friends. Now that it’s down, let’s take a look back at our guesses of the trajectory and see what we got wrong, and what we know about the real trajectory now that we know the landing site and the time of the landing. First off, note the real landing site, compared to the landing site that was identified prelaunch Real landing site/time Lat = 44.12 deg N. Lon = 19.51 W @ 13:11:18 UTC. Reported site/time Lat = 43.07 deg N. Lon = – 31.05W @ 13:40 UTC Real landing site with the bullseye to the east, prelaunch reported site to the west.
So what does this tell us? As we suggested in our earlier posts, the reported landing site could not be achieved at the landing time from a 90 deg inclination orbit. The actual landing site, however, could be (and was) achieved from 90 degrees. Let’s check out then, what it must have been (LRO orbit in magenta, LADEE orbit in Blue, neither on the same side during the landing):
And ten minutes before:
So we didn’t need a different inclination, 90 degrees was fine. With the proper landing time and site, we would have had a really good estimate of the trajectory. It’s all “basic geometry, and we know about that!”
Finally, here’s the local terrain looking from the southwest.
Again, really cool work by the Chinese Chang’e 3 Team!
Astrogator_Mike With our last post, we identified the overall nature of the Chang’e 3 trajectory, now let’s try to narrow it down a bit to see what the landing approach might look like. Firstly, we should add to the previous post. You might have noticed in the last posting:
We show here a lunar arrival from the North. That’s not the only available approach. We could also approach from the south and get the same inclination:
Which gives us two possible approaches to the landing site. Our current information has the spacecraft approaching the site from the south, so we can switch things to accommodate that. Our Chinese friends announced that they did achieve LOI at 6 Dec 2013 09:53. This time represents the conclusion of a 361 second burn, which places the center of the burn at 9:50. That’s where we can put our impulsive LOI maneuver. Once there, we’ve been told C3 circularized in a 100 x 100 km (altitude) orbit. From there we are told (from Robert Christy @Zarya_info): 1. The periselene was dropped to 15 km on Dec 10 13:20 UTC 2. The periselene will be further dropped to 2 km on the orbit before landing. 3. Landing will take place in Sinus Iridum with coordinates 43.07 deg N Lunar Latitude, 31.05 deg W Lunar Longitude. 5. Landing will take place Dec 14 13:40 UTC with the landing start at 13:26 UTC from periselene Can we deduce the landing profile, and thus the inclination from this? Perhaps. Note that all press so far has referred to this orbit as merely “polar”. While we might assume this means exactly 90 degrees, I don’t think it can be 90 if we stick with the landing site and landing times we list above. See below that if we assume a 90 degree inclination, we can’t get to the appointed landing site at the appointed time (bullseye represents identified landing zone):
Note the time in the lower left. Lowering and raising the orbit won’t help, the Moon simply hasn’t rotated under our orbit plane at the landing time. How confident are we of the orbit plane? Pretty confident. The cislunar transfer is relatively fixed. We know the launch time, launch site, perigee location and the transfer time to LOI. We know (roughly) the capture aposelene altitude, so we’re only left with inclination to play with. Could there be a plane change somewhere after LOI? Sure, but this seems like a pretty unlikely fuel cost, especially when we can just get what we want by changing our inclination. Another way of looking at this is to check it out in inertial space:
This makes things a bit more clear. Our orbit plane is pretty inertial (note the orbit plane is pretty fixed over a week of time in orbit since LOI). We just have to wait for the Moon to rotate underneath. If we land on the 14th at 13:40, our site just isn’t there yet. However, if we change our inclination to about 105 degrees:
Again with the inertial view:
We can see that a bit of inclination gives us just what we need, a relatively “polar” orbit, a ground track over the site, and a landing time that’s about right. Let’s look again at what’s the view of Earth during landing:
Pretty good geometry, all 3 major Chinese ground stations well above the horizon for many hours. So what are the sources of errors here? Many. We certainly don’t match the AOS and LOS times published. Those can easily be explained by the fact that we don’t know the actual parking orbit dimensions. We’ve been assuming 100 x 100 km circular (and we’ve played with that a bit to make things be timed right) but we’ve got 50+ revs in orbit for errors to build up, and we this assumes a perfect insertion at 100 km periselene, and a perfect insertion. We also don’t know precisely what altitudes were reached with our periselene lowering maneuvers, nor where the first periselene lowering maneuver was targeted (15 km at first periselene after the burn, or 15 km 20 revs later?) So we’ve got a lot of slop. Still, let’s assume that our landing time and landing site are right, and let’s see where a couple of our US satellites are that we know pretty well. [Disclaimer: While I (Astrogator_Mike) was the trajectory lead during the cislunar phases of LADEE, I am currently only very very part time on the mission as offsite support during science ops, and right now at this very minute I am blogging on my spare time on SEE company computers. The trajectory information I am using for both LADEE and LRO is readily available on the JPL Horizons site and comes from there. Thus, no NASA funds, computers, data or assets of any kind were used in the making of this blog posting and I am doing this in my spare time.] So, where are LRO and LADEE? Based on spice files from the wonderful aforementioned JPL Horizons site, here are where our US orbiting robots are during the Chang’e 3 landing:
So let’s step through this a bit close to landing and see what our geometry is.
Let’s get a bit closer to the landing site, and see if LRO or LADEE can see the site:
Of course LADEE has no camera on board (except the star trackers) but it won’t be able to see anything anyway. LRO, on the other hand, has a decent horizon view of the landing and might be able to see something against the star field. So from LRO we have:
Of course this all assumes that the times we have are right, but if LRO could somehow scan the area over the landing site during the right pass, they might be able to see something. Regardless, good luck and godspeed to the Chang’e 3 controllers! Astrogator_Mike
Our Chinese colleagues launched a lander to the Moon on December first, but unfortunately they have chosen not to publicly share where their spacecraft is. A few days ago there were several TLEs in Spacetrack associated with the Chang’e 3 launch, all of which didn’t appear to be associated with it at first glance (wrong plane, etc.) . So, given we don’t have any real ephemeris available, let’s see if we can create a reasonable guess on our own with a bit of Astrodynamics detective work. First, let’s start off with some information we do know from their live broadcast. We know the launch time: 1 Dec 2013 17:30 UTC. We know the launch site is the LC2 Launch Complex at the Xichang Satellite Launch Center (XSLC). I have 28.2455 deg N Latitude, and 102.027 E Longitude for that site. Next question is, what direction do they launch, and to what altitude? Robert Christy’s excellent site Zarya.info provides us with a decent first guess here: Robert did a lot of our work for us by nailing the separation events, and approximate latitude and longitude positions of events based on the video stream. It may seem rough to try to calculate a trajectory from this information, but actually it tells us quite a bit. We know the launch site, and we know the approximate perigee altitude of the transfer trajectory (~210 km) . We also have a pretty good idea of the TLI time: 6 Dec 2013 09:30 UTC from a tweet by Robert Christie (@Zarya_Info) and we know the landing site from the same source. So let’s make a few simplifications: Impulsive maneuvers. I’m going to use these for TLI and LOI for now, just because I’m lazy and don’t feel like digging out the parameters of the spacecraft (and it makes my setup a bit more complicated). From Robert’s link about, I can eyeball the center of TLI at about 17:45:36 UTC on Dec 1, 2013. That’s where I’m going to put my TLI. I don’t know the exact launch azimuth they flew, so I’m going to guess 97.5 and then let it float a bit (i.e. use the burnout Lat, Lon and Alt as controls). I don’t know their exact burnout altitude, so I’m going to guess 210. Normally I’d know all of this stuff exactly. If I were planning the mission (as I did on LADEE) I knew my launch site, azimuth etc. and the exact burnout state of the Mintoaur V. I could figure out from this what my launch time ought to be, and when TLI was etc. In this case, I’m having to guess things from parameters I DO know. It’s detective work, but my peers in China have to work with the same physics and math as me, so it’s going to be pretty close. So I have to fix the launch time and the TLI time, let the burnout conditions float a bit for my controls, and then vary my TLI DeltaV to hit an LOI at the proper time and get into the proper orbit (I’m going to use a 100 km altitude, 90 deg inclination orbit). So what does that give us? First off, it makes our launch ground track look like this:
TLI occurs at the end of the yellow segment, burnout of stage 2 at the end of the red segment. So assuming a 90 deg inclination, 100 km altitude insertion (impulsive still) on 6 Dec 2013 9:30 UTC, we get a trajectory that looks like this:
This gives us a good idea where C3 is now, but what does the rest of the trajectory look like? First let’s look at the LOI geometry.
Note that with a 5 day transfer(4.8 really, 116 hrs) the approach to the Moon comes from the side, with respect to the Earth. This is a nice geometry for visibility at LOI, especially for a polar orbit, because it lets the LOI burn happen in full view of the ground. With equatorial spacecraft (LADEE) getting the LOI in view of the Earth can require a bit more work. It’s not a great geometry for watching the maneuver, given that there won’t be much radialrate component, but it’ll do. Now let’s take a closer look at the Earth to see what is visible.
Without digging up the locations of the ground stations, it’s pretty clear that major portions of China are visible, as is Australia. Since we know Chang’e 3 is using some ESA stations, this is set up for a multiple ground stations to see LOI. Nice geometry for Orbit determination and realtime tracking of the event. After one rev in Lunar orbit, we can see what the orbit looks like here:
The next question is, how does this set us up for landing? We have approximated the landing site at the Sinus Iridum region, with a Lunar Latitude of 43 deg N, and a Lunar Longitude of 31 Deg W. Note the lighting of that site at LOI:
Let’s look at the first day’s worth of ground tracks on the Moon, which will help us see what we’re waiting for, both in terms of lighting and geometry:
Note that the light blue line shows the incoming trajectory and the subsequent lines show the progression of ground tracks (which move from right to left). Further note that part of our ground track is in shadow (blue) as is the landing site, and part is in sunlight. Obviously, for landing we’d like sunlight both on the site and on our ground track. Here are the tracks a day later:
Our sunlit ground track on the right is moving closer to the landing site, and the shadow is drifting in the right direction as well. The trick here is to just wait in orbit while the Moon rotates under us. Looking at this in 3D gives a better geometrical perspective:
The orbit is pretty much fixed in inertial space, and we just have to wait while the Moon rotates. If we wait until Dec 15th we get this:
At this point we’ve all but gotten lined up with the landing site, and it’s time to start the descent. Now we have to do a bit of guessing. We know that the descent profile goes from a 100 km circular orbit to a 100 x 15 km orbit (altitudes). We know that the vehicle lowers to periselene and then lowers from there. We’re going to assume that we won’t go a full rev in the 100 x 15 km orbit, but will instead just execute one half rev and descend. If so, it looks like this:
It’s hard to show on this scale, but if you zoom and look closely at the left, you can see the orbit starts at 100 km (yellow) and then descends to 15 km on the right. Let’s look from the landing site perspective. Note we can see the approach hyperbola still (blue) the 100 km parking orbit (yellow) and the spacecraft at Periapsis just peeking over the limb at the top. You can see that the parking orbit isn’t completely locked inertially, it’s got a bit of drift in it from the Lunar gravity field.
Now I have to really fake it. According to the superb site Spaceflight101, the landing engine actively throttles all the way down:
Spaceflight101 Chang’e 3 Flight description
While I can model an engine that throttles, it’s way too much work (if I was working on the mission, I’d have the lander controls people do this) so I’m going to fake it with 2 constant thrust finite burns and a coast segment. I won’t bother trying to get masses and engine masses right either, I just want to show the basic idea:
Of course the real profile won’t be exactly like this, but this is a reasonable facsimile. Let’s check out the geometry with respect to the Earth:
And finally let’s see what’s visible from Earth at the landing time:
Which looks pretty darn good if you want to get coverage from Chinese ground stations. (Note: I lit the Earth up a bit in this picture to show what was visible, but this half of the Earth is in darkness at the landing.) Pretty fun stuff. We welcome any updates, if anyone has better data than we do, it’s real easy to change the assumptions and rerun. Astrogator_Mike
Part of an astrogator’s job is to determine the spacecraft’s current orbit, and predict where it will be in the future, just as the navigators on sailing ships figured out where their ship was and where they were going. Those navigators used star sightings, Sun observations, and accurate clocks to figure out their latitude and longitude. One of the ways they calculated their speed was to drop floats into the water and time how long it took for the ship to move a measured distance. On LADEE we also take observations and measurements to figure out where LADEE is. These measurements are called tracking data, which we receive from many ground tracking stations which are positioned around the world. We use large dish antennae from NASA’s Near Earth Network, NASA’s Deep Space Network, and from the commercial Universal Space Network. We schedule time each day for the various ground stations to track LADEE, using radio signals, and they send us tracking data files containing their measurements during and after the pass. In these files we can get the ground station’s observations of the distance to the spacecraft (“Range”); the speed at which the spacecraft is moving towards or away from the ground station (“Doppler” or “Range Rate”); and the angles in the sky where LADEE is, from the ground stations’ pointofview. We don’t always get all these types of measurements, nor do we get tracking data all the time, but we don’t always need to. (We will never say no to more tracking data, though. We like it when the controllers schedule extra time to communicate with the spacecraft because then we get more tracking data! We often exclaim, “More Data!”) After we get the tracking data, we use a first guess at what we think the orbit is currently, and we estimate a new orbit by adjusting the trajectory slightly to fit the new measurements. We use AGI’s Optimal Extended Kalman Filter, (in Orbit Determination Tool Kit, aka “ODTK”) to read these files and estimate LADEE’s orbit. We’ve used this on many other cislunar and Earth orbits before, and it really works great! The end result of our orbit determination work is a spacecraft ephemeris file of where LADEE has been in the past, and another ephemeris file of the predicted orbit, which is where we think LADEE will be in the future. The ephemeris file of the past trajectory is sent to the scientists who need to know where LADEE was when it took their science measurements. The predicted ephemeris file is used by the mission planners for scheduling their activities. It’s also used by other astrogators to calculate “acquisition” data to send to the ground stations so they know where and when to point their antenna to track LADEE. And it’s used by other astrogators to plan the next orbit maneuvers and attitude orientation plans. It’s very important that we calculate accurate orbits, and we have some pretty tight requirements on how accurate our past orbit knowledge must be, as well as how accurate our predicted orbit must be. As you might imagine, since the tracking is done using radio waves, the signals can have noise on them. The signals are affected by things like weather (one of the ground station dishes was struck by lightning a few weeks ago!). The electronics on the spacecraft also are affected by the harsh temperature changes in space. To make sure our orbit is accurate we spend a lot of time “tuning” the filter settings. This includes identifying and throwing out bad data, calculating how much noise is on each measurement, and calibrating bias values for the various tracking electronics. Also, every time there is a maneuver, whether a large orbit burn, or a small momentum dump, we have to calibrate that maneuver and estimate its exact magnitude and direction. It’s been very rewarding working with the other LADEE astrogators that do this orbit determination work: Craig Nickel, Ryan Lebois, and our Orbit Determination lead, Lisa Policastri. They have done a great job, preparing for years before we launched, and since have been working long hours on crazy shift schedules during operations to make sure we know where we are and where we are going! We have a lot of discussions on how the data look, what the biases might be, and things to try to make our orbit solutions better. (Some conference papers we’ve written describing the details of how we’ve done Orbit Determination for other missions can be found at http://www.applieddefense.com/resources/whitepapers/ )
After we get an orbit solution, we then go through a lot of selfconsistency checks to convince ourselves that our orbit is good, and we check our previous predictions with new data to see how well we are doing (as shown in these figures.) It is frustrating, though, that we can’t just look out a window and see where LADEE really is! Sometimes it seems like we are flying a remote control airplane with a blindfold on, maneuvering by only listening to the sound of the engine as it gets closer or farther from us! Every once in a while, though, we get a good indication that things are going well. For example, when we were getting ready for our first Lunar Orbit Insertion burn, we were sure everything was going well, but there’s still a lot of anticipation in the air…. we were leaving the Earth’s dominating gravity, and falling rapidly towards the Moon. (“Falling with Style” as Buzz Lightyear would say!) We designed LADEE’s trajectory to go behind the Moon and—based on our predictions—we planned the exact time for the main engine to fire to brake into Lunar orbit, igniting just a few minutes after LADEE became visible again from behind the other side of Moon. We sure hoped we got the prediction correct! In addition to estimating the time LADEE would lose signal as it disappeared behind the Moon, we also estimated the uncertainty in that time; we predicted we knew the time within 2 seconds. We were listening to the other team members on the voice loop, and we cheered as they called out that the Loss Of Signal was within 2 seconds of our prediction!
Then came the Lunar Laser Communication Demonstration (LLCD experiment), a great deep space technology that has now been successfully demonstrated. (A cool video here: http://youtu.be/ptfLfrWI648 and the NASA web page is here: http://llcd.gsfc.nasa.gov ?). When they started the first experiment, it just worked! As quoted in the article from Popular Mechanics: (http://www.popularmechanics.com/science/space/nasa/lunarlasercommunicationexperimentsucceeds16068586): “We thought the ground terminal would have to do a little searching, but it turned out it was pointed perfectly,” Boroson says. “We turned it on and all cheered.” The connection was almost instantaneous. After the spacecraft and ground terminal connected, a 4inch laser beam travelled 238,000 miles from the moon to New Mexico. And in the article from Spaceflight Now: (http://spaceflightnow.com/minotaur/ladee/131023laser/#.Ummt_mTh8F): Over the 239,000mile distance between the Earth and the moon, the 4inchdiameter laser column disperses to a width of 3.5 miles by the time it reaches the ground. There was really little room for error: the pointing had to be correct, and the predicted ephemeris has to be accurate. Although we had done several tests prior to launch, sending test products to check out the system, we didn’t know how things would work until they turned on the LLCD system. You can imagine when we heard over the voice loops and in the status briefings last weekend that the orbit ephemeris was good enough that the system worked right away, and that they didn’t need to search, we were very excited!
The orbit determination team really did their job! And, in addition, our nineperson Flight Dynamics Team performed several other tasks to make the LLCD experiment work. We calculate the orientation (also called the “attitude”) of the spacecraft for the experiments. We also create the onboard spacecraft ephemeris so the LLCD instruments mounted on LADEE know where and when to point back at the ground terminals on Earth. And we generate the pointing angles for the ground terminals to point their LASERS at LADEE. Of course, we’re not the only ones… Our flight dynamics team sits in the room next to the activity planners, and the many subsystem engineers, and we are near the controllers, and the many other folks that worked through the weekend and over long nights at Ames to make this successful. It was an exciting weekend! And that’s just listing some of the folks at NASA Ames. To see the rest of the LLCD team, check out the web page http://llcd.gsfc.nasa.gov – It really is great to see what can be accomplished when so many people, of very different talents, have a chance to work together, and try something new. Sorry for the delay in updating, Astrogator_Mike had to make the long drive home after LOI3 and get configured back in his home base. In the mean time, Lunar Orbit Insertion Burn 3 (LOI3) was completed successfully (within 0.6% of target) on Oct. 13, 2013. LADEE’s post LOI3 orbit had an aposelene altitude of 250 km, and a periselene altitude of 235 km. You can see below that this has evolved over time to 220 km x 260 km. LADEE will now stay parked (i.e. no maneuvers) for roughly a month, while the spacecraft does alternating Lunar Laser Communication Demonstration (LLCD) tests, and calibration tests of the other science instruments. In fact, the LLCD has been doing really well, breaking records and having all sorts of fun: NASA Is Now Communicating With the LADEE Spacecraft Via Laser LADEE’s current view looks like this:
Which looks like this from above the orbit:
And from the Earth looks like this:
Note that you can zoom in on any of these pictures by clicking on them. Our Japanese friend on twitter @LadeeOrbiter posted this picture today:
This is way cool. It would make a great Halloween costume! We understand that the twitter account is an unofficial site for lunar impact flash even monitoring by amateur astronomers in Japan to support the LADEE mission. The LADEE effort to involve amateur astronomers all over the world is supported by NASA, and I’d give you the link to their site about this, except that the site (like the rest of the US government) is offline. So try this link instead. We also have been told that the LADEE girl in the picture ( the LIMEM@STER) is a parody of a Japanesemade game called THE IDOLM@STER. You can see a bit of that here. The LADEE Lunar Orbit Insertion burn 2 (LOI2) executed as planned this morning at 3:38 PDT, placing LADEE into a 4 hr orbit. Things move much faster now for the spacecraft, and the Moon is looking a lot bigger. We originally captured with a periselene altitude near 560 km but our periselene has now been lowered to an altitude of ~235 km by Earth perturbations in the PostLOI1 24 hr orbit. The planned periselene of the commissioning orbit was 250 km, however the small (<1%) underperformance of LOI1 caused aposelene to be slightly higher, and thus we got slightly more Earth perturbations than we nominally planned for. The result of this is that we got a bit of free lowering from the Earth, which we’ll take! (Since we plan to go lower than 250 km anyway). So the current plan is to drop the aposelene to 250 and perform commissioning there in the 235 x 250 km orbit. LOI2 lowered our apogee down to ~2200 (we’ll have to wait for some more tracking to verify that exactly). From our preLOI2 planning, things should now (9 Oct 2013 13:00 UTC) look like this:
And we are here in the orbit:
If you could see the orbit from Earth you’d see this:
Lunar Orbit Insertion Maneuver 2 (LOI2) is upon us, scheduled for 09 Oct 2013 10:38 UTC. This maneuver will lower our periselene altitude from 15700 km down to 2220 km and change our orbit period from 24 hrs to 4 hrs. The maneuver will last for 220.8 seconds, and will impart a deltaV (change in velocity) of 293 m/sec. Right now LADEE sees this view:
And the orbit from above would look like this:
From Earth, if you could see the orbit, you’d see this:
Go LADEE! LADEE is now in its last rev in the 24 hour capture orbit, and preparing for LOI2, which will lower the spacecraft into a 4 hr orbit. LOI2 is scheduled for 10:38 UTC (3:38 AM PDT) Wed. morning, Oct. 9. Here’s the view from LADEE to the Moon:
Here’s the orbit [Note: blue shows the 4 hr orbit we’re going to next. Dotted lines show the past trajectory, solid are into the future. So we’re not quite at aposelene yet.]
And finally the really cool view AstrogatorJohn came up with yesterday of the view of the orbit from the Earth:
So if you go outside tonight and see the Moon, imagine this orbit. After posting the picture of the Moon from the parking lot at Ames, we thought it would be cool to see what LADEE’s orbit would look like, if we could see it, from the Earth. The picture below is from the Earth to the Moon, with Ecliptic North at the top. The White Orbit is our current orbit, and the small white circle is where LADEE was when I took this snap… it’s moving to the right, towards periselene; the Blue Orbit is what it will be after LOI2, and the Green Orbit is the near circular orbit we will stay in during commissioning for about a month before we start science operations.
Astrogator Mike is in the Flight Dynamics Room planning our second lunar maneuver, Lunar Orbit Insertion2 (LOI2), and I (Astrogator John) am processing tracking data doing orbit determination. Mike noticed the Moon and Venus over the parking lot, so I went out there with him took this picture with my phone. That’s Venus to the left of the Moon.
The LADEE Spacecraft successfully performed Lunar Orbit Insertion maneuver 1 (LOI1) on Oct. 6, 2013 3:57 PDT. The LOI1 maneuver captured LADEE into a 24 hr orbit. After 3 days (and 3 revs) in the capture orbit, the spacecraft will perform LOI2 on Oct. 9 at 3:37 PDT. The second of 3 Lunar Orbit Insertion maneuvers, LOI2 will reduce LADEE’s orbit down to a 4 hr orbit. Finally, LOI3 will be performed Oct. 12 at 8:00 PM PDT to circularize the spacecraft in a 235 km orbit. LADEE will spend a month in this “commissioning” orbit, while the spacecraft is checked out before fulltime lunar science begins, and the LaserCommunications experiment will be tested.
At this time (7 Oct. 2013 7:53) LADEE is past its first aposelene, and is headed for its first periselene after capture.
The LADEE spacecraft is now in Lunar orbit. Tracking data will later confirm the precise parameters of the orbit, but based on telemetry of thruster performance and accelerations, the LOI1 burn appears to be close to nominal. The planned Lunar orbit has an orbit period of 23.1 hrs. The next planned maneuver (Lunar Aposelene Maneuver 1, or LAM1) is scheduled for the 2nd aposelene, which would occur roughly 1.5 days from now. For LOI1 results close to nominal, this maneuver can be waived. LOI2 is nominally scheduled for 3 revs after LOI1. Watch the Lunar Orbit Period and Lunar Apoapsis Altitude come down once the Lunar Eccentricity goes below 1.0 (from Hyperbolic to Elliptical). The Moon is now under control. Based on LADEE’s altitude (below 66,000 km) the Moon is now the primary gravitational body acting on the spacecraft. In other words, the Moon’s gravity is now stronger than the Earth’s.
This picture really shows the change the Moon is imposing on the orbit, which until now had been a large elliptical orbit around the Earth:
Note that the white arc LADEE is currently on turns red when LADEE gets below 50,000 km. After that, you can see another short, white arc on the trajectory which is Lunar Orbit Insertion 1, or LOI1. Here’s LADEE’s view of the Earth:
And finally, the approach trajectory:
You can see the LOI1 arc in this view as well. About 15 hrs to LOI1 now…. As we mentioned previously, we’re not quite within the Moon’s sphere of influence yet. (LADEE will be within most definitions of the Moon’s sphere of influence by 19:30 UTC today, October 5th.) Even so, we’ve been modeling the significant effects of the Moon’s gravity on our trajectory since we launched. The way we modeled it, as is standard, was as if the Moon is a perfect sphere. In reality, however, we know from all the previous lunar missions that the Moon’s gravity field is quite “lumpy” and when we are in orbit around the Moon, we will model the Moon’s gravity with many more equations than we did when LADEE was close to Earth. As we approach the Moon, we have to transition from considering the Earth’s gravity as dominant to the Moon’s gravity as the primary effect. For trajectory design purposes we’ve been switching from an Earthcentered orbit propagation to a Mooncentered orbit propagation when LADEE gets within 50,000 km of the Moon’s center. (Our analysis has shown that this number doesn’t have to be very precise to meet the accuracy requirements. On the Clementine lunar mission we didn’t switch to a Mooncentered orbit propagation until we captured at Lunar Orbit Insertion.) In addition to calculating the trajectories, we also have to track LADEE and estimate the orbit, using a technique called “Orbit Determination.” Fellow Astrogators Lisa Policastri, Ryan Lebois, and Craig Nickel work with us on this. The method we use is an Extended Kalman Filter, which processes tracking data sequentially as we receive the data from the tracking stations around the world. Orbit Determination is sort of like curve fitting, and one of our jobs is to estimate the trajectory that best fits the tracking data. As you can see from the pictures we’ve posted previously, LADEE’s trajectory bends a lot as it goes from the Earth’s influence to the Moon’s. To model the changing gravity for Orbit Determination, we decided to do something different than we do for trajectory design. Instead of switching from EarthCentered to Mooncentered at a specified point, a few days ago we started running two algorithms sidebyside; one Earthcentered, and one Mooncentered. We trend the two different orbit estimates, and by the time we reach the LOI1 maneuver (6 Oct 2013 10:57 UTC), which is just past periselene, we will be ready to transition to using the Mooncentered algorithm for the rest of the mission. LADEE continues to approach the Moon, now nearing 100,000 km in altitude.
Note the last few parameters on the left. Lunar orbit period is zero (hyperbolic still), as is the Lunar Altitude of Apoapsis. The Lunar Altitude of periapsis isn’t accurate either, as the spacecraft is still mostly in Earth orbit. The Lunar disk is getting larger, and the Earth disk smaller:
This shot shows the upcoming portion of the trajectory, when the Earthbound trajectory is taken over by Lunar gravity:
The final shot is the best, our Lunar approach:
LADEE is rapidly approaching the Moon. Depending on who you talk to, you can consider the spacecraft to be within the “Sphere of Influence” of the Moon somewhere near 66,000 km (on LADEE we switch central bodies on our numerical integrators at 50,000 km, but that’s not a magic number). So we’re not quite MoonCentered yet, but that doesn’t stop us from giving you pictures in a Moon centered frame. As you can see, showing the Earth orbit no longer has great utility:
[Note: Velocity is still Earthrelative] I have to still show my favorite view of the phasing loops, the EarthMoon rotating coordinate frame, but Earthbound phasing loops are about to be less relevant.
But as much as I like the phasing loops, this is the view we really should be thinking about (and I like it so much I just tweeted it!):
And this view gets me very excited:
But we still can look back to where we came from:
If you check the dates on the pictures, you can see what order I created them in, as the dates don’t all match and I’m animating in real time. Today in the Flight Dynamics Room at Ames, fellow Astrogator Craig Nickel called out when LADEE became closer to the Moon than to the Earth – at 10:07 PDT tonight – and it’s not coming back!
LADEE passed perigee this morning near 4 AM PDT and is now headed for the Moon. Currently the spacecraft is above GEO, with the TCM1 maneuver coming at 3 PM PDT today (1 Oct. 2013)
LADEE now under the GEO belt, and heading for its last perigee.
Next Maneuver: TCM1 on 1 Oct. 2013 22:00:00 UTC (11 hrs after Perigee 3). On Sep. 28 2013 05:33 UTC, LADEE is coming out of its last apogee and at an altitude of 214,000 km.
Perigee occurs on 1 Oct near 11:00 UTC. A final small midcourse maneuver will take place at 1 Oct 2013, 22:00 UTC. This 0.9 m/sec maneuver will precisely target insertion parameters for the 6 Oct. 2013 10:57 UTC LOI1 maneuver. LOI1 is designed to place the spacecraft into a 24 hr orbit, with a periselene altitude of 590 km [correction: previously I said 750 km, this isn’t quite right. For LADEE we aren’t capturing right at periselene, like orbital mechanics would recommend. Instead we burn off periselene just a bit. We wait until 5 minutes past we come out from behind the Moon, and start our burn. This ends up being roughly 5.5 minutes after periselene. This allows the Deep Space Network to get a lock on us and telemetry to start flowing before the burn starts. So the altitude at the end of this burn is at about 750 km, but the actual periselene altitude is closer to 590 km]. After 3 revolutions in this orbit, 3rdbody Earth gravitational perturbations will have lowered periselene to an altitude of 250 km (by design). At this point, LOI2 will be performed on 9 Oct 2013 10:37 UTC ( to place LADEE into a 4 hr orbit (also with a 250 km periselene altitude). LADEE will spend 3 days in this orbit until LOI3 (12 Oct 2013 10:37 UTC), which circularizes the orbit at 250 km. LADEE will spend 30 days in this “commissioning orbit”, and will also perform tests using the laser communications experiment (LLCD). The timing and magnitudes of the maneuvers leading to the commissioning orbit are given below.
Executed Maneuvers: AM1 11 Sep 2013 23:00:00.000 9.34 m/sec PM1 13 Sep 2013 16:36:08.000 16.96 m/sec PM2 21 Sep 2013 11:53:19.000 17.492 m/sec Planned Maneuvers TCM1 01 Oct 2013 22:00:00.000 0.9 m/sec LOI1 06 Oct 2013 10:57:00.210 329.86 m/sec LAM1 07 Oct 2013 22:51:32.205 0 m/sec (error corrections for LOI1) LOI2 09 Oct 2013 10:37:55.651 295.99 m/sec LOI3 12 Oct 2013 10:37:34.993 238.56 m/sec Here’s a quick LADEE update for Sept. 22, 2013. The LADEE team performed a second Perigee maneuver yesterday (21 Sep. 2013, 11:53 UTC) to raise LADEE’s orbit to have a period of 10 days, and to set up the spacecraft for Lunar capture on Oct. 6. LADEE’s path to this point is shown in dotted lines, while the upcoming trajectory is shown as solid. Note that LADEE is now in phasing loop 3, and will continue around a full orbit that will conclude on October 1st. LADEE will then begin the final portion of its trajectory, the 5 day trip to the Moon which concludes on Oct 6 with Lunar Orbit Insertion burn LOI1. No further deterministic maneuvers are required (only a small TCM to correct out statistical errors from PM2) before the LOI phase begins. So even though LADEE has a full Earth orbit left, it is Moonbound. LADEE is still in an elliptical orbit of the Earth, but at the next apogee LADEE will encounter the Moon.
Many people have asked about LADEE’s trajectory, which uses 3 and a half “phasing loops” to get to the Moon. On one of my other postings, a reader asked if phasing loops saved deltav on the translunar injection (TLI) burn. The answer is no. The cost (in deltav) to get to a lunar transfer from a specific injection orbit (for example the 6.4 day orbit LADEE currently is in) is the same if you go direct as it is if you go around a few times first. The savings come elsewhere, in particular with the cost of correcting for errors from the launch vehicle (rocket). There are four important reasons why phasing loops are being used for LADEE. 1. Mass The Minotaur V couldn’t throw the whole mass of LADEE all the way to Lunar Injection. 2. Launch Dispersions Let me borrow from my answer in the comments section on a previous post: The Minotaur V, which is a stack of 5 solids, isn’t considered to be a particularly precise rocket. In other words, if we were to ask for a 6.3 day orbit, we might get a 5 day orbit, or we might get an 8 day orbit. In a direct injection trajectory (such as the 3day missions used by Apollo), injection errors can only be corrected out after good amount of tracking can be done (~ 24 hrs normally) to determine the orbit (OD, or “Orbit Determination”). However, as the spacecraft gets further and further away from the Earth, the cost of correcting out launch errors gets larger as well. Often times, by the time enough tracking data can be gathered, the cost of correcting out any launch errors can be 510 times the actual size of the error. So a 5 m/sec error would take 25 m/sec to correct, etc. If, instead of using a direct approach, you use phasing loops the cost is a lot closer to 1:1 (i.e. a 5 m/sec error in launch costs 5 m/sec to correct, or can even save you fuel). It’s not a pure 1:1 ratio, because there is a timing aspect as well, but in terms of the energy of the orbits, it is 1:1. Assume that you’re going to launch to a 6.4 day orbit and that you’ll then transfer to an 7.6 day orbit, and then a 10 day orbit, and then spend 5 days getting to the Moon (total of 29 days). The cost of transferring to the 5day lunar transfer from the 6.4 day starting orbit is always the same. Now say that your rocket doesn’t give you exactly what you want, and instead of a 6.4 day orbit, you are inserted into a 7 day orbit. Instead of doing a TCM to correct out that error, you simply replan your trajectory profile. You spend 7 days in the first orbit, but instead of transferring to a 7.6 day orbit, your first maneuver is zero, and you stay in the 7 day orbit for 2 days. So your first rev is 7 days, second rev is 7 days, and then you transfer to a 10 day orbit, and take 5 more to get to the Moon (still 29). Same thing if you are launched to a 5 day orbit. The second orbit can be 9 days, the third 10, and 5 days to the Moon (29 days total again). You get the picture. The total deltav to get to the Moon doesn’t really change, but your orbit profile is flexible to large dispersions in your injection. Phasing loops have been used on many other missions (Clementine and WMAP are 2 good examples). I designed the phasing loops on LADEE to accommodate the Minotaur V dispersions. The LADEE spacecraft barely had enough fuel to do its science mission, and the choice of phasing loops allowed the mission to accommodate the Minotaur V dispersions, at the cost of some extra time in cislunar space. The operations costs are not free (of course), but if you can’t fit on the rocket, sometimes you don’t have a mission. [Funny thing is that although the Minotaur V is “supposed” to have large dispersions, the fact is that the launch last Friday (Sept 7, 2013) was just about perfect. We got almost precisely the nominal trajectory, in what probably is the most precise injection a Minotaur rocket has ever done. Had we known in advance that we could have gotten such an injection, we probably would have gone direct.] So here are a few examples of how phasing loops allow you flexibility. As stated previously, LADEE was launched into a 6.4 day orbit. However, let’s say LADEE got into a 5 Day orbit instead: If LADEE had been launched into a 5 day orbit (green), we then could have raised the 2nd orbit to have a 9.5 day period (blue), and the third to have a 9.8 day period purple and then done our normal 5 day transfer to the Moon. The two pictures below tell the story. On the left the orbit is shown in an EarthMoon Rotating coordinate system. The Earth is in the middle, and the Moon is stationary from the top. Imagine that you’re way above the EarthMoon system, and that you are slowly rotating at exactly the same rate as the Moon goes around the Earth. On the right is the normal view, an Earthcentered inertial frame.
If LADEE had been launched into a 6 day orbit (green), we then could have raised the 2nd orbit to have an 8.3 day period (blue), and the third to have a 9.9 day period purple and then done our normal 5 day transfer to the Moon.
If LADEE had been launched into a 7 day orbit (green), we then could have raised the 2nd orbit to have an 8.1 day period (blue), and the third to have a 9 day period purple and then done our normal 5 day transfer to the Moon.
If LADEE had been launched into an 8 day orbit (green), we then could have raised the 2nd orbit to have an 8.4 day period (blue), lowered the third to have a 7.7 day period purple and then done our normal 5 day transfer to the Moon. The 8 day orbit and above starts to cost more energy, because you have to lower the 2nd orbit and then raise it back up for the third. So in this case, while the rocket would have placed us in a higher orbit than we wanted (and thus you’d think it might save us energy) we end up having to pay a bit extra to get the timing right.
Note here that all the examples I show have us keeping the time of the third perigee mostly constant, along with the time of flight between that perigee and the Moon constant at 5 days. This comes from the fact that once we’ve launched and the Minotaur Stage 5 has fired, our line of apsides (between apogee and perigee) is mostly fixed in space (actually it was fixed before launch for optimization purposes, but that’s another topic) and we are now locked into getting at the Moon when the Moon is at the same latitude as our apogee. 3. Widening the Launch Window Another thing phasing loops give you are a wider launch window. With the argument of perigee (and thus the line of apsides) fixed before launch, we are fixed to arrive at the Moon when it as a specific latitude (same as our apogee). Given that, a direct launch would have only had a very short launch period if you assume that you’re always launching with the same energy from the upper stage. Phasing loops allow you to widen the window up to 5 days. In the case of LADEE, we actually launched on the first day of the launch period (on the first second of the launch window) but we were lucky. We’ll take the luck, but we didn’t plan for it. Instead, we had a 5 day window. On the first day of the launch window (Sep. 6, 2013), our first orbit would be 6.4 days, the 2nd 7.95, the third 9.95 and then about 5 days to the Moon.
On the second day of the launch window (Sep. 7, 2013), our first orbit would be 6.33 days [Note: the rocket is always launching us to the same orbit, but the Moon’s gravity alters our orbit a bit, so the first rev doesn’t always have the same period] , the 2nd 7.00, the third 9.95 and then about 5 days to the Moon.
On the third day of the launch window (Sep. 8, 2013), our first orbit would be 6.24 days, the 2nd 6.32, the third 9.55 and then about 5 days to the Moon.
On the fourth day of the launch window (Sep. 9, 2013), our first orbit would be 6.19 days, the 2nd 6.27, the third 8.82 and then about 5 days to the Moon.
The last day of the launch window (Sep. 10, 2013), our first orbit would be 6.16 days, the 2nd 6.32, the third 7.95 and then about 5 days to the Moon.
Why does the launch period stop? Look at the rotating frame picture in each of the examples. Think of the picture in terms of quadrants, with the first quadrant being in the upper right, second in the lower right, third in the lower left, and 4th in the upper left. Any loop in the first quadrant gets to apogee with the Moon in front of it. This is fine, because the gravity of the Moon will give us some extra velocity at apogee, and will raise our subsequent perigee altitude. The closer we are to the EarthMoon line (the vertical white line in the rotating frame picture), the more boost we get from the Moon. The further away we are from the Moon, the less boost we get. Going into the 4th quadrant is bad, because if we get in front of the Moon at apogee, then the Moon’s gravity slows us down, and drives the perigee altitude into the Earth. In the 2nd quadrant we get slight gravitational lowering at perigee, and the 3rd we get slight gravitational raising. If you watch the sequence through the launch period, you see that each day the first loop clocks further (clockwise) to the right, closer to the 2nd quadrant. We have to launch to get our orbital plane to match the Moon’s on arrival, and also have to make this happen when the Moon has the same latitude as our apogee. This is all important for the trajectory planning of LADEE, because when you launch off a rocket from the Earth, your insertion perigee is usually low (200 km). You don’t want to come back at this altitude the next time around. So we launch when the Moon will raise us (without requiring a maneuver at apogee, which we could also do, but we’d rather not require a maneuver at the first apogee to keep the spacecraft from hitting the Earth). So as long as our first loop stays within the first quadrant in the rotating frame, we’re OK. This gives us a 45 day launch window (some times we lose the first day if we decide that potential launch dispersions will throw too many statistical cases into the 4th quadrant.) 4. Flexibility after launch The phasing loop plan is also very robust in the face of missed maneuvers. A missed PM1, for example, can easily be accommodated by modified PM2 and PM3 maneuvers and still get to the Moon at the same time. A missed PM2 is can be accommodated by waiting another month in orbit, and achieving LOI1 in November. The ability of the plan to easily be modified in the face of contingencies is another strong feature of the phasing orbit approach. In the pictures below, we see what happens with a missed PM1. The spacecraft stays in 6.4 day orbit for a second rev, and then raises to a 11.25 day orbit with a 41 m/sec maneuver. At the final perigee (Pf or PM3) we execute a 8 m/sec maneuver to bring apogee down to Lunar altitude.
The plan is also robust to a missed PM2 maneuver. This profile would require LADEE to wait an extra month in Earth orbit. The gray orbits indicate the first month. We show the trajectory starting after PM1 moving towards PM2. Once PM2 is missed, the spacecraft spends 2 more revs in the grey (moving through the 4th quadrant) and then the approach pattern starts again.
Phasing loops offer several advantages to the mission planner. At the expense of longer operation costs, phasing loops have offer a reduced TCM budget in the face of large launch dispersions, expanded launch windows, and overall robustness to contingencies. 

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“Back of the Envelope” Astrogation: Recreating the New Horizons Trajectory
A “Star Wars” Rebel astrogation Officer does some “back of the envelope” work
As I was watching the great success of the New Horizons team, I became motivated to do a bit of quick “back of the envelope” calculations to recreate the trajectory. I don’t have to start completely from scratch, because in 2004 I created an STK/Astrogator tutorial giving the basic ideas of how to set up the New Horizons trajectory:
Astrogator New Horizons Tutorial
I thought it would be fun to update things and make them closer to what was actually flown. I can easily do so because the New Horizons Astrogator Yanping Guo (along with legendary Astrogator Bob Farquhar) gave me what I need in this paper:
Yanping Guo and Bob Farquhar: New Horizons Mission Design
I will refer to this from now on as “Yanping’s paper” just for simplicity, but Farquhar helped write it as well.
I’m going to do this in STK/Astrogator, but the basic idea would be similar in other software. I’ll update my scenario a bit to include the launch portion along with the published Bplane parameters at from Yanping and see if our geometry lines up with hers. (STK/Astrogator was actually used for the New Horizons mission, which makes this even more relevant. It was also used on Messenger, LRO, LCROSS, LADEE, etc… but I digress.)
Launch Targeting
Firstly, let’s get the launch set up, so that I can hit the right time of the launch coming out of KSC. The Launch vehicle used was an Atlas 551, a beast of an Atlas with 5 solid boosters, a Centaur upper stage, a Star 48B on top and the 5 meter fairing. That’s actually one heck of a stack of stages. Here’s a really cool report of the launch events, according to Jonathan McDowell:
Jonathan’s Space Report No. 560
“The powerful Atlas 551 rocket, with five solid boosters, roared off the Florida pad after two days of delays. The solids separated at 1 min 45s into launch, arcing into the mesosphere before falling to Earth. The 5meterdiameter fairing separated at 3min 23s, followed seconds afterwards by the two pieces of the CFLR (Centaur Forward Load Reactor), a contraption that connects the smaller 3.1mdiameter Centaur to the fairing for structural stiffness. By this time Atlas was in space, with the fairing probably reaching an apogee of 150 km or so. Atlas shut down at 4min 27s, falling away 6s later, and the Centaur second stage ignited at 4min 33s as the trajectory flattened out, reaching orbit insertion at 1910:08 UTC with a 167 x 213 km parking orbit. The vehicle coasted for 20 minutes and restarted over South Africa, with a 9min burn taking the Centaur to 800 km altitude at a velocity of 12.4 km/s, a hyperbolic Earth orbit which will take the Centaur out to the asteroid belt. At 1939 UTC the spintable on the forward end of the Centaur began to rotate, and the injection stage with the payload separated. The injection stage is an Alliant (Thiokol) Star 48B solid motor, the same motor used on Delta 2 third stages and on the old Shuttle PAMD flights. Solid kick motors like to be spinning when they fire to even out any misalignment of the thrust direction, hence the spin table – although the Star 48B also has a set of small hydrazine rockets to correct any unwanted nutation. After the Star 48B burn, the payload had reached escape velocity not only with respect to the Earth but also relative to the Sun (The velocity was 16.2 km/s relative to the Earth and I estimate an asymptotic velocity of 12.3 km/s, corresponding to 42.6 km/s relative to the Sun and leading to a heliocentric eccentricity of around 1.05)”
(You should follow Jonathan on twitter: @planet4589 and you can find the latest version of his “Jonathan’s Space Report” here: Jonathan’s Space Report)
I have to divert a bit from my deep space trajectory because I’m geeking out about the Atlas 551. That’s a sweet rocket. Let’s see a picture of the stack from the launch press kit:
New Horizons Atlas 551 Launch Stack (From NH Launch Press Kit) Click to Enlarge
Ok, let’s just look at rocket itself. (You really want to click on this one, it’s a cool rocket!)
New Horizons Atlas 551 (5 meter fairing, 5 solids, 1 RL10 on the Centaur) [Click to enlarge]
The Star 48B is a very reliable (and available) upper stage, and stacking it on top of a Centaur is pretty unusual, but necessary for the high C3 (157.64 km^2/sec^2). That C3 is (as noted by Jonathan) hyperbolic with respect to the Sun!
Let’s take a quick look at the staging profile (also from the press kit):
Launch Events (1 of 2)
[Click to Enlarge)
Launch Events (2 of 2)
[Click to Enlarge)
Our purpose here is to duplicate the interplanetary trajectory, so I’m not compelled to completely duplicate the launch segment. I’m going to model all burns as impulsive burns (I don’t have their engine models anyway) and I’m going to combine the Centaur and Star 48B into one insertion burn. It’s fine to do this, since ultimately the multiple insertion burns are just targeting a single trajectory after launch, with a single defined asymptote. The Centaur and Star48 burns were optimized to hit a single asymptote, so I’ll just model that part.
From my NH tutorial mentioned earlier, I will reuse these asymptote conditions:
2006 New Horizons Asymptote (from Trajopt)
These conditions came originally from Trajopt (an old DOS program written at SAIC) and they’ll be good enough. I could have gotten them from a variety of other sources that help you search for planetary swingby opportunities. I’ve used MAnE, Trajopt and “Swingby Calculator”, and there are many others. Regardless, these conditions are plenty good and they ought to get me to the Jupiter swingby, and then I’ll work from there.
So I will launch out of KSC with these conditions:
Astrogator Launch Burnout Conditions
In STK/Astrogator, we model the launch as a portion of an ellipse that starts at the ground and then meets the launch insertion state. This is a decent estimate of the burnout state. After the launch, we’ll coast in orbit for a bit, and then execute an escape maneuver. The mission control sequence for that looks like this:
STK/Astrogator Single Targeter to hit outgoing Asymptote
So I’ll vary my launch time (to get the orbital plane, or the Right Ascension of the asymptote) , my coast duration before the impulsive escape deltav (to get the Declination of the asymptote) and the deltav itself (to get the C3, or energy) to hit the asymptote conditions. When I do that, I get this type of a flyby at Jupiter:
New Horizons Trajectory with Asymptote only.
So using the Trajopt asymptote does actually create an encounter with Jupiter, but I don’t get anywhere near Pluto. According to Yanping’s paper, my flyby should look like this:
New Horizons Jupiter Flyby (from Yanping’s paper sited earlier) [Click to Enlarge]
But if you go into the Jovian system for my flyby, you’ll see this:
Asymptote only targeting, Jupiter flyby side view
Asymptote only targeting, Jupiter flyby side view
So that tells me that the asymptote isn’t going where I want. I can fix that pretty easily. Yanping gives me the Bplane parameters I need at Jupiter to continue on the Pluto. If I match these parameters, I should then be close enough to an encounter with Pluto that Astrogator can target me the rest of the way in. I’ll match them by slightly varying my departure asymptote parameters.
The Bplane is a fictional plane that is used for precise targeting during a gravity assist or for planetary orbit insertion. It can be best thought of as a bullseye or target plane attached to the assisting body. The trajectory’s intersection point on the Bplane is where the spacecraft would go if the swingby planet had no gravity. This turns out to be useful because Bplane targets behave very linearly as you move the trajectory around (while targeting) while the actual periapsis point (or closest approach point) doesn’t move very linearly near the planet due to the nonlinear force of gravity.
The Bplane is defined to be the plane that contains the focus (usually the center of mass of the body) of an idealized twobody trajectory (assumed to be a hyperbola) that is perpendicular to the incoming asymptote of that hyperbola. The incoming and outgoing asymptotes, S and O, and the focus of the hyperbola are contained in the trajectory plane, which is perpendicular to the Bplane. The intersection of the Bplane and the trajectory plane defines a line in space. The Bvector is defined to lie along this line, starting on the focus and ending at the spot where the incoming asymptote pierces the Bplane. A reference vector (R) is used to externally define the other planar axis. There are different choices to use for R. Typical examples are the planet’s orbit normal, or the planetary pole vector. You can use whatever you want, as long as you specify what it is (so others can duplicate what you’re doing, like I’m about to do)
Bplane Definition
The vectors T and R lie in the BPlane and are used as axes. The coordinates of our point in the coordinate system defined by those axes are called BdotT and BdotR, and they are the standard parameters given that allow you to target a swingby.
My initial state from Trajopt gives me the right direction for my transfer trajectory to get close to our Bplane targets (i.e. somewhere in the Jovian system), but I’m going to substitute in the Bplane parameters from Yanping’s paper instead of those that Trajopt originally generated. This should get me close enough to Pluto to hit our Bplane targets later.
I will target the following at Jupiter (From Yanping):
BPlane Target:
B dot T = 342421 km
B dot R = 2629560 km
Jupiter Periapsis (closest approach) time = 28 Feb 2007 12:00:00.000 UTC
(Jupiter’s North Pole Reference frame)
I’ll use these parameters for now, and then let them be varied later. On the real mission, Yanping used trajectory correction maneuvers (planned for up to 25!), and didn’t try to accurately hit the Pluto Bplane precisely all the way back from launch. I can get away with that here, so I will. If I wanted to simulate how a real mission would do it, I’d truncate off my asymptote solution back at Earth, and our Bplane targets at Jupiter and recover from those errors with TCMs. In a numerical simulation, I can pretend that I can hit targets much more precisely than I can in real life, so I’m going to cheat here and do that.
I will use a doublenested targeter to achieve our goals. The inner targeter varies the Launch Time, the Coast duration, and the Injection deltav to achieve the asymptote conditions. The outer targeter will vary the asymptote conditions of the inner targeter (RA, Dec and C3 of outgoing asymptote), in order to achieve the desired Bplane parameters and arrival epoch at Jupiter. So I’m going to let the targeter vary my first guess at the outgoing asymptote from Earth (the guess that came from Trajopt) in order to hit the Bplane parameters that Yanping says I need. The Astrogator MCS for this is below:
STK/Astrogator Mission Control Sequence with Double Nested Targeters
After this converges, my trajectory looks like this (view at Pluto closest approach):
New Horizons Trajectory with Jupiter Bplane Targeting
[Click to Enlarge]
Which is a lot closer. The Pluto arrival date isn’t exactly right and while it looks close on the solar system scale, I am actually 5.9 million km from Pluto at periapsis. This shouldn’t surprise me though, because I haven’t really targeted anything at Pluto yet. I am relying solely on the Jupiter Bplane parameters to get us there. At the Jupiter flyby, my geometry looks like this:
Bplane Targeting (double nested), Jupiter flyby top view [Click to Enlarge)
Which looks a lot more like the encounter geometry that Yanping showed in her paper. So now, I’d like to actually target my Pluto periapsis to the right spot and at the right time to match the encounter.
Again, I’ll rely on Yanping’s paper to tell me what I want to hit:
BPlane Targets:
B dot T = 10910.6 km
B dot R = 2041.9 km
Pluto Periapsis (closest approach) time = 14 Jul 2015 11:58:59 UTC
(Pluto orbit normal frame)
I will target this with a triple nested targeter (highly bogus in terms of trajectory realness in this case, but cool anyway). It looks like this:
Triple Nested Targeter: Hitting the Pluto Bplane all the way from Insertion
1. The deepest internal targeter (Target Launch Asymptote) varies the launch time, coast duration, and burn deltav to hit the outgoing asymptote (RA, Dec and C3 of asymptote)
2. The second targeter (Target Jupiter Bplane) varies the outgoing asymptote conditions of the deepest targeter in order to hit Bplane parameters at the Jupiter swingby.
3. The outermost targeter (Target Pluto Bplane) varies the Bplane parameters at the Jupiter Swingby in order to hit the desired Bplane parameters at Pluto.
This setup is simple but powerful and gets an answer, but I couldn’t really do this when flying a mission. It essentially has me targeting the Pluto Bplane accurately from conditions all the way back at insertion in Earth orbit! Launch vehicles can’t hit the asymptote RA and Dec within 0.000001 degrees, nor can injection maneuvers be executed with precision of 10e6 meters. I’m going to ignore that though, since I know I’d have to do midcourses, and just enjoy the coolness of the trajectory.
So in my uberprecise mathematical universe we get this at arrival:
Pluto Periapsis Geometry
From Yanping’s paper she has the geometry looking like this:
Pluto Approach Geometry (Gua and Farquhar)
We can also look at both sun occultations to see if they match up:
Pluto Occultation of Sun
Charon Occultation of Sun
And they do (which is pretty satisfying!) Of course our fellow Astrogator Yanping Guo had to do things much differently than this, since she had to correct out insertion errors, attitude dumps, and Orbit Determination (OD) errors, etc. all along the trajectory for 9.5 years! In fact while they had planned 25 Trajectory Correction Maneuvers (TCMs), they only had to perform 9, which saved them 2/3 of the planned deltav. This gives them plenty of deltav to use to retarget to a Kuiper belt object later this year (pending additional NASA funding). Once they announce the target KBO object, I’ll update and extend my trajectory to match.
Also, I think the final conditions at the encounter may have been slightly off from what I have here (due to TCMs, adjustments, etc. that occurred after the paper was written). Once I get my hands on those conditions, I can trivially retarget things to achieve those states instead of what I hit above. (and I will, and will update here). What I’ve found so far has been conflicting, so I’ll stick with the paper. If someone has better data, pass it on. It’s easy to redo.
I end this fun with a bit of animation showing the Plutonian system in action. I’d been wanting to see an animation of the system with the dualplanets coorbiting, so I just made one myself. I love seeing Pluto dancing around the system barycenter. Planet and moon positions come from JPL SPICE files.
I’ll put the STK scenario up shortly, and post a link to it here when I do. If you’d like an ephemeris in a nonSTK format, email me and I’ll create one for you.