The End Part II

Okay this really is the last post. I just want to nip in the bud, right here, right now, shutting down this site was my idea. No one, and I mean no one, asked me to shut it down. I received some comments regarding some top level manager's opinion on my recent posts on the T7 issues (which I should point were temporary and have been fixed). It was a mistake for me to even discuss them here, even in the vague manner I tried to convey, and their disapproval was brought to my attention. This issue scared me. It was fun when this site was just a small group of people who wanted to hear the latest from Cassini. But if I need to be concerned about what I write, then it becomes less fun. I love what I do, I can't imagine myself doing any better at this point in my life, and I will not jeopardize it for a blog. I'm sorry, but I won't. And rather than look over my shoulder and wonder if what I just sent is kosher with everyone who are higher up than me, I'd rather just end this page. I apologize to all those who have come to rely on this page. I really do. Don't stop caring about the Cassini mission just because I'm not here to blog about it.

Now, that's not to say I am completely going away. Last night, I decided rather than give up here and do nothing with volcanopele.blogspot.com, I will just change the format. I have had this novel, essentially in my head for 5 years now, waiting for me to actually commit it to paper. I've decided to write it here on this blog. I'm not sure how this will work but I think it will be an interesting experiment. Based on similar projects on Blogger, I will post a segment of the novel every few days, once a week or so, on a post. It could be a chapter, it could be more, it could be less. I personally like that concept. So I am going to give it a try. So on September 24, this blog will be replaced by "Afterword". I hope some of you come back for that.

The End

This will be the last post of this blog. I know a lot of you have come to rely on this site for information on the Cassini mission, but it appears that I will no longer be able to continue posting here. Ironically, this site was killed by its success. This site was read not only by people in the public, but by those in the Cassini project as well. I knew full well of this, but apparently I crossed a line with one of my posts last week, and they called me (litterally) on it. This site was only going to stay up as long as I got something out of it and you did too. Now, this site has become a lot less fun. So, effective immediately, I will no longer be posting on this blog. I will probably post occasionally on the Unmanned Spaceflight.com forum, but will likely become a lurker. I will keep the site up for the next week, when I will then shut it down for good :-(

New Titan Image: Canyonlands on Titan

The Cassini RADAR team released this view of Titan taken last week during the T7 flyby. This cutout from their SAR noodle is located near 55 degrees South, 7.5 degrees West and is approximately 300 km long. Unlike the previous image, the channels in this region consist of long valleys (up to 200 km long and 200 meters deep) that have only a few tributaries. These channels are more akin to river systems on earth rather than the arroyos seen in the T3 swath and in the previous image.

New Titan Image: Titan's Rain Drains to the Plains

This is the second of three views released by the Cassini RADAR team showing portions of the RADAR SAR swath returned last week. This portion is from south central Tsegihi near 48 degrees South, 14 degrees West. This view extends 240 kilometers from left to right. At top, you can see a deeply incised channel flowing from a region of bright, rough terrain down to darker, smoother material. This fits with the view that methane rains wash material from the bright highlands down to darker plains. Near the bottom of the image, there is a branching network of channels, with the widths of the channels varying. These properties are suggestive of rainfall run-off channels rather than river networks.

Still, note how well this liquid has eroded these channels. These are quite deeply incised, suggesting either that the liquid efficiently erodes the bedrock, or these channels have been active for a good percentage of geologic time.

New Titan Image: Shoreline on Titan?

The RADAR team on Cassini has released some of their SAR swath taken on September 7. I will post my comments on all three cut outs. This portion is near the very end of the part the were able to get back. The second half was lost. This portion shows a possible shoreline in the central part of the dark albedo feature known as Mezzoramia. On the left, you can see terrain that is suggestive of erosion by liquids, with alcoves and scarps. At right, the surface is quite dark suggesting that the area is much smoother than any other place so far looked on Titan by Cassini RADAR. Many of the bright features that bound this terrain are similar to shoreline terrain on Earth.

This portion of the swath is from 66 South, 356 West in central Mezzoramia. This portion is 330 km wide and 175 km tall.

Cassini Significant Events for 09/08/05 - 09/14/05

Haven't mentioned one of these in a while, but this week's Cassini Status update is now online. Regarding the mishap during last week's Titan flyby:

A significant amount of science data was lost during the recent Titan flyby as a result of an operational problem at the DSN tracking station, and a software error on the spacecraft. The software error was the larger contributor of the two causes, and the data loss resulted from an improperly set flag preventing the spacecraft from writing to or reading from the A side of the solid state recorder, so the result was performing the encounter with only half of the expected data storage volume. Commands will be sent on September 15 to reset the flag to its proper value, and normal operation is expected after this. The nature of the code error is now fully understood and has been reproduced in the spacecraft test bed. A decision will be made in the near future whether to correct the flight code or to implement workarounds to prevent the conditions that led to execution of the faulty code.

These problems led to the loss of all data after 1 minute prior to closest approach (because the "B" recorder was full at that point) as well as our high resolution mosaic, VIMS' medium resolution mosaic, and the RADAR inbound altimetry data. We did, however, obtain our global mosaic (a portion was released publically earlier this week) and RADAR received a portion of their SAR swath over central Tsegihi, Mezzoramia, and some features a little farther to the east.

New Telesto Image: Squinting at Telesto

CICLOPS has released this processed view of Telesto, taken on August 1 from a distance of 768,000 km. From that distance, the 24-km wide Telesto appears as nothing more than a blog of light with no discernable features or shape. Believe it or not, this qualifies it as one of the best images of Telesto thus far (Voyager's best image was ~ 5km/pixel) But, fear not, better images of Telesto are coming. Cassini comes within 9800 km of this small, trojan satellite on October 11, 2005. This will be one of the closest flybys of a small satellite during the tour. At closest approaches, images with a resolution of 56 m/pixel are possible (~425 pixels across Telesto's disk).

Off-topic: Cassini finally sees spokes in Saturn's B-ring

Not exactly satellite-related, but as has been alluded to on a few discussion sites in the past week, the Cassini Imaging team announced today that they had finally observed the spokes, first seen by Voyager but had not been seen by Cassini. The spokes appear to be bright wispy features on the B-ring in the above image and in the images released today. These images are of the unlit side of the ring, so the B-ring appears dark due to its opacity and the C-ring, at lower left, appears bright. Saturn's limb can be seen toward the upper left corner. Pretty neat stuff.

New Titan Image: Monitoring Fensal-Aztlan

CICLOPS has released this mosaic of the Fensal-Aztlan (formerly known as the "H") region on Titan. Fensal is the northern branch of the "H". Fensal has some subtle brightness variations and has quite a few bright spots, or "islands", dotting the region. Their distribution appears to be more scattered than similar sized bright spots in Shangri-la, west of Xanadu. There, the spots were clustered into several "archipelagoes" and aligned in a similar fashion, usually east-west. The spots in Fensal don't seem to have a prefered orientation. A few larger bright spots can be seen in Fensal, including Bazaruto Facula on its eastern end.

Aztlan, the southern branch of the H plus the dark region surrounding Elba Facula to the east (not in this particular crop), has far fewer smaller islands, but does have several large islands, including Sotra Facula, a 240 by 120 km sized bright feature just right of center in the lower left frame, and Coats Facula, a smaller island to the east of Sotra.

This mosaic is just 4 frames within a larger, 20-frame mosaic to be released later. This mosaic was taken during last week's T7 encounter.

DPS Titan News

Emily Lakdawalla at the Planetary Society has posted on her blog quite a few notes from the Titan DPS talks. Unfortunately, not much is news to me so it is rather difficult for me to remember what has been publically mentioned and what is new. It is a great read and and I definitely recommend checking it out.

New Rhea Image: Frame-Filling Rhea

CICLOPS today released this processed image of Rhea taken on August 1, 2005. This image was taken from a distance of 255,000 km and has a resolution of 1.5 km/pixel. As the title suggestion, this image was taken when Rhea nearly filed the entire narrow-angle camera field-of-view. Nothing shocking from Rhea, just lots and lots of craters (with a few fractures up at the top toward Rhea's wispy terrain). This image primarily shows the southern trailing hemisphere of Rhea. Two prominent impact basins, ~300 km across can be seen along the terminator. The top basin is unnamed but the second basin is Izanagi. This basin was the site of one of the pre-launch artwork done for the Cassini mission. No sign of the fractures shown in that rendition.

T7 Coverage Map

CICLOPS has released the coverage map for today's flyby of Titan. Cassini ISS will examine the sub-Saturnian hemisphere of Titan, particularly around the Fensal-Aztlan region (formerly known as the "H"). The coverage for this encounter will primarily come from two mosaics. The first, MONITORNA001 outlined in green, is a 2 km/pixel mosaic over the entire visible disk. This is similar to other full-disk mosaics from Ta and T3. The second mosaic, COMBINED001 outlined in red and yellow, is a higher resolution mosaic consisting of many images near the center of the visible disk. Key targets for this mosaic include features within Fensal, Aztlan, Quivira, and northern Tsegihi regions, such as Bazaruto Facula (with its 80-km central crater), Omacatl Macula, and the debris deposit in northeast Aztlan that bisects Quivira.

A map showing RADAR SAR coverage is also available.

New Dione Image: Older Southern Fractures?

CICLOPS released today this processed view of Dione on August 1. This image was taken from a distance of 269,000 km and has a resolution of 2 km/pixel. The wispy terrain of Dione can be seen toward the top with Padua Linea running from top center to right and Palantine Linea running along the terminator at left. In contrast to these relatively sharp fractures, the fracture systems near the south pole, just to the left of the large impact basin, have relatively subdued topography and are probably older than the fractures that make up the wispy terrrain. The radial feature near the center of the disk, Cassandra, was thought to be caused by a ray crater, but analysis of the topography associated with the feature now shows that Cassandra likely has a tectonic origin.

Note the two craters just to the left of Cassandra. These craters have a similar shape to Ali Baba and Aladdin craters on Enceladus, perhaps indicating local heating in that region of Dione, in order to produce the viscous relaxation we observe.

New Look

The formatting and column issues have bothered me (and others) for the last time. I have switched to a different template within Blogger to see if that helps, but a few features from the old template, like recent posts, are now gone :( I will try to fix that soon enough.

Titan-7 Flyby Info

View of Titan from Cassini 2 hours into ISS' high resolution observation, about 3 hours prior to closest approach (sub-spacecraft point=4.4N, 26.2W). The plot was generated in GISS' Titan 24 software. The map is derived from ISS map released in March (ask for full version used here, just adds blank space north of 34N). The full version of above plot is available as well as one with feature labels. The data for plot was obtained from Mission description document.

T7 Quick-facts:

• Closest approach occurs on September 7 at 1:33 am PDT
• Closest Approach Distance = 1075 km (bumped up from 950 km)
• Relative speed WRT Titan = 5.9 km/sec
• Closest Approach Lat and lon = 67 South, 308.1 West
  
• South Polar Pass with sub-Saturnian hemisphere visible inbound
  
• Outbound flyby (sunlit inbound)
• Phase angle at -3hours = 51.5 deg.

RADAR SAR and ISS imaging highlight the science plans for tonight's T7 flyby of Titan. This is the 8th flyby of Titan out of 45 planned for the nominal mission. The 7th flyby, T6, took place on August 22, and yielded plenty of data for CIRS and MAPS, but not much for the other remote sensing instruments. However, during T7, RADAR, ISS, and VIMS make up for lost time.

This flyby is lower than the August flyby, with Cassini coming within 1075 km of the surface of Titan. This is higher than the originally planned 950 kilometers. Many of the 950 km flybys may have to be similarly raised due to higher atmospheric densities at higher altitudes than expected. As you can see in the above plot, Cassini will once again look at the sub-Saturnian hemisphere of Titan on its inbound leg. This hemisphere has been in view of the last 3 flybys, but have no fear, Cassini will return to the anti-Saturnian hemisphere and the Shangri-la region during T8 in late October.

ISS controls the spacecraft for much of the period prior to closest approach. Two large mosaics are planned. The first is a mosaic at about 10 hours out. This should have similar coverage and resolution to the global mosaics taken during Ta and T3, global with a resolution of about 2 km/pixel. The second is a higher resolution mosaic taken from 5 hours out to about 1 hour out. The coverage map for this mosaic should be out soon, but this mosaic would have enough time to build up a large mosaic with similar coverage and resolution to those taken on Ta and Tb. Overall this is shaping up to be one of the better flybys for ISS in some time. Phase angles are similar to those from the past few orbits, higher than those from Ta-Tb-T3. Lots of interesting features at the center of the disk including Bazaruto Facula (with an 80-km wide crater at its center), Quivira with its possible channels and a debris deposit bisecting the feature and flowing into Northeast Aztlan, and Omacatl Macula.

RADAR is back for T7. So far, RADAR has acquired two SAR (synthetic aperature radar) swaths, first on Ta and again on T3. Both swaths covered portions of the northern leading hemisphere. On this encounter, RADAR SAR will acquire a swath over the southern sub-Saturnian hemisphere. I have produced a coverage plot for this swath, though I would ask that it not be reproduced on other sites. The swath starts out in north central Tsegihi, an area of bright terrain, which appears to be similar to Xanadu but slightly darker in albedo. Like Xanadu, Tsegihi is a region of mottled terrain, though with less contrast than Xanadu. Continuing along, RADAR will run into Mezzoramia, a "dinosaur-shaped" dark region that maybe a temporary reservoir of seasonal rainfall run-off from the south polar region. Images of Mezzoramia from July of last year indicated a possible difference in how sharp the southern and eastern boundary is compared to the western and northern boundary. It will be interesting to see if such a difference is detected in the RADAR coverage of the region. The SAR swath continues to as far south as 77 degrees south Latitude, even farther south than Ontario Lacus, a 235-km wide dark feature that maybe a lake. Many of the lake-like features near the south pole appear to concentrated on the leading hemisphere side of the pole, though this could be an emission angle effect (surface contrast improves as you approach the sub-spacecraft point). So RADAR SAR may miss most of the larger "lakes", but smaller features, like those seen on Ta, are possible. T0 images reveal a possible dark feature that maybe similar to Ontario Lacus to the southeast of Mezzoramia, near 70 South, 330 West, so that might be something to look out for. The eastern half of the SAR swath is in a region not seen very well by Cassini ISS (best pixel scale ~ 35 km). This region could be very similar to the area seen by RADAR on Ta, with a lot bland terrain puntuated by the occasional volcanic center.

RADAR also has altimetry and radiometry on this pass. Altimetry will cover the bright-dark southern boundary of Chang-tu at the far eastern end of the RADAR SAR swath. There should be altimetry at the far western end as well, checking for topography associated with Shiwanni Virgae and north-central Tsegihi. Hopefully, the altimetry won't show a slope to the east this time ;-) RADAR Radiometry will look at the thermophysical properties of the northern anti-Saturnian hemisphere, to compare with results from Ta, which looked at the northern sub-Saturnian hemisphere. This data, taken after closest approach, will cover the region that will be seen by RADAR SAR in late October during T8, an east-west swath that will cover central Belet and central Adiri. This region will also be see quite a bit by the remote sensing instruments, like ISS, later in the mission.

Of course, other instruments will gather data during this encounter. UVIS has their second star occultation of Titan's atmosphere, this time using alpha Pegasus (Markab). UVIS will be using the occultation to look for N, N₂, and hydrocarbons at various latitudes. This is a "glancing" occultation since the star will not pass behind the limb of Titan, only the upper atmosphere. The December 2004 occultation of lambda Sco allowed UVIS scientists to detect various hydrocarbons like methane, acetylene, diacetylene, ethane, ethylene, as well as Hydrogen cyanide in Titan's atmosphere as well as measure the abundances of those species. VIMS is prime for almost 4 hours on approach to Titan, starting around 8 hours and 45 minutes before closest approach. This will allow VIMS to create a full-disk mosaic similar, but at lower resolution, to our MONITOR mosaic taken shortly before VIMS' MEDRES observation. VIMS will also take a few snapshots near closest approach northeast of Shiwanni Virgae. CIRS and the Fields-and-Particles instruments will also be active on this encounter. CIRS will be continuing to look for variations in the distribution of hydrocarbon species both temporally and spatially. The MAPS instruments, like MAG and MIMI, will continue to examine the interaction between Titan and Saturn's magnetosphere.

Playback of T7 data takes place during two playback periods. The ISS images of the surface will be returned tomorrow night and Thursday morning and should show up on the JPL raw images page Thursday afternoon, PDT. The rest of the data will be played back starting at around 5:30 am Friday morning, PDT and will continue until around 2 pm PDT. Images from this period, mostly from after Closest approach, should be on the raw images page Friday evening. RADAR SAR data will be played back during this playback period, so don't expect any data from them to show up until at least Monday, and even that is pushing it. Given the weekend and the fact that a number of RADAR team members are in transit from the DPS conference that takes place this week, I wouldn't expect any images from the RADAR team until at least Wednesday. I know that's a long time, but we should have patience with the RADAR team in getting their data assembled.

DPS News and Notes

The AAS' Division of Planetary Sciences Conferences is taking place as I type in Cambridge, England. No, I am not there. But the Planetary Society's Emily Lakdawalla is and she has a great blog post with some of the results from yesterday's Cassini talks. Among the highlights include Larry Soderblom's confession that the DISR mosaics may have north off by as much as 15 degrees counter-clockwise, which is a major relief for me given my work to try to find the landing site in ISS images. Given their current understanding of "north", I could not find any site that matched orientation of the islands seen in the DISR images. Now with this revelation, there is a solution (easternmost tip of Adiri). Larry also mentioned the planned coverage by RADAR SAR of the landing site in T8. This swath is an east-west pass across central Belet and Adiri. The RADAR team extended the Beam Three path (at the expense of altimetry) to try to cover the landing site, but the signal/noise ratio maybe a bit low, I'm afraid. Hopefully, something good will come out of it and we can start making sense of all our data. FYI, RADAR SAR swaths are composed of five beams (you may have noticed the seams in early RADAR products). Beam three is the center beam and has the best signal to noise ratio. The Principal Investigator of the HASI instrument on Huygens reported that his instrument found a number of inversion layers in the Titan thermosphere. This confirms the INMS result that showed a number of waves in the methane and temperature profiles in the upper atmosphere. Apparently this wave structure continues down to at least 510 km. Now why is this so important... The SSP and the Permittivity Sensor on HASI both detected slight changes in conditions at the surface after landing. The increase in permittivity and changes in the speed of sound and spacecraft tilt maybe related to the vaporization of methane by Huygens as it sat on the surface, but that is just one possibility.

There were a number of results from the instrument teams from onboard Cassini. Many of the major results announced today were related to the rings and Saturn, and rightly so since admittedly they have gotten very little press coverage compared to the satellites so it is good they have their day in the sun. But this is a blog about the satellites, so who cares about those results ;-) Most of the Enceladus results were announced earlier at a press conference but some instrument teams did clarify them. VIMS last week announced they had found crystalline ice (absorption band at 1.65 microns) and simple organics (absorption band at 3.44 microns). During his talk, Bob Brown mentioned that the aborption band is attributed to a C-H stretch. In other words, it is some kind of organic compound, but VIMS can't tell what it is with just this one absorption band. Brown also announced that VIMS had not found any ammonia on Enceladus, shutting the door on ammonia-water volcanism. I'm not sure I agree with him there, but we may want to look at models that don't include ammonia. This also fails to explain how INMS saw N₂. The CIRS principal investigator, Mike Flasar reported on results from Enceladus. In addition to the hotspot in the south polar region, CIRS found a relatively low thermal inertia, indicating that Enceladus is covered in unconsolidated material. Perhaps due to infalling E-ring material.

Finally, the RADAR team presented their results from T3. The most interesting features in that swath were the numerous linear to sublinear dark streaks, nicknamed cat scratches. These features have been interpreted as linear or longitudinal dunes, similar to those found in Saudi Arabia and Australia (near "Lake" Eyre). However, the RADAR team has been comparing the scratches to icy dunes in Antartica, which are visible in RADAR images of the continent, but not so much from the ground. The dunes take the form of changes in grain size rather than topographic features that one could see from the ground. Such an interpretation would jive with ISS' inability to resolve the scratches if both the dunes and the material that fills in between them are dark at 938 nanometers.

RADAR also released an image yesterday showing these dunes and a couple of drainage channels west of the "Circus Maximus" impact basin.

New Janus Image: The Two Faces of Janus

CICLOPS has released this view of Saturn's moon Janus taken on August 2. This view shows only a slim crescent of Janus lit by sunlight, highlighting a couple of craters near the terminator. On the left side, however, Janus is dimly lit by Saturn, to the left of this image. Several large impact craters are visible in the Saturn-shine.

Janus is a small, irregular satellite of Saturn, only 181 km across. Cassini's closest encounter with Janus won't come until the very last day of the nominal mission, June 30, 2008, when Cassini is scheduled to come within 45,000 km of the surface of this satellite. Cassini flew within 50,000 km of another small satellite of Saturn, Pandora, yesterday for Cassini's closest encounter with that satellite during the nominal mission.

Pandora Rev14 Non-Targeted Encounter

Today, Cassini will come within 52,000 km of the surface on one of Saturn's small, inner moons, Pandora. Pandora acts as one of the shephards of the thin F ring, orbit just outside of the ring. Pandora is a small, irregular, with a diameter of 114x82x62 km. Voyager views of Pandora's surface showed a ancient, heavily cratered world, but Cassini views, like the one above, suggest that, though heavily crater, small-scale topography may be subdued, perhaps due to F ring material mantling the surface.

This encounter with Pandora, while not a targeted flyby, will provide our best views of the satellite thus far and at 52,000 km, this will be the closest Cassini will come to this satellite. The best possible images from Cassini at closest approach would have a resolution of 300 m/pixel over the satellite's trailing hemisphere (assuming that it rotates synchronously which I believe it does).

Images and other data from this non-targeted encounter should be returned tonight or tomorrow.

More New Titan Names

The IAU's Working Group for Planetary System Nomenclature (WGPSN) has approved 12 additional names for features on the surface of Titan. These include names for various albedo features on the surface of Titan, including the northern H region. Two additional types of features are included in this round of names, like Arcus (arc-shaped features) and large ringed features, ring-shaped albedo features that are currently thought to be craters. Some of the highlights in this round of naming include:

• The feature previously nicknamed "Pelopennesos" is now known as Oahu Facula. This feature is similar to the other bright "islands" in Shangri-la, but appears to be connected by a narrow isthmus to Dilmun.
• The bright, Arc-shaped bright feature, associated with a very bright spot at 5-microns, has been named Hotei Arcus.
• The feature previously nicknamed "Manhattan" (because it is shaped like a big apple) is now known as Texel Facula. This feature is located at the far eastern end of Antilla Faculae in western Shangri-la.
• The VIMS "snail", interpreted by the VIMS team as a possible volcano (or cat feces, depending on who you ask), is now Tortola Facula.
• Several ring-shaped features have been named, including two in eastern Shangri-la near its boundary with Xanadu (Guabonito and Veles) and in north-central Tsegihi (Nath).
• The northern H region is now named Fensal. A possible name now for the H region as a whole could then be "Fensal-Aztlan"

The USGS site now has a map with names.

Enceladus Animation

The Photojournal has an animation with a wrap-up of the results from the July flyby, showing both the effects of Enceladus on Saturn's magnetic field as well as showing the great images and fantastic mosaic produced during the encounter. Definitely worth checking out.

Arcus on Titan

The IAU's Working Group for Planetary System Nomenclature (WGPSN) has approved the feature type, Arcus. This term will be used for arc-shaped albedo (possibly topographic as well) features. This feature type would applicable to such features as the "smile", found to be very bright at 5 microns by VIMS.

No word yet on additional names for Titan and this "arcus".

New Tethys Image: Tethys in the Dark

CICLOPS has released this processed view of Tethys taken on August 3, when Cassini was 842,000 km from the satellite. Only a thin crescent was visible of Tethys at the time this image was taken, when the phase angle was 144 degrees. Images like these can be used to study the photometric properties of the surface material on Tethys, particularly with how backward scattering it is. Two good sized craters can be seen along the terminator, or the dividing "line" between night and day. The one at about the 3:30 position is Penelope. The smaller crater near 5:30 is Antinous. While it hasn't been stretched to make it visible, much of the left part of Tethys' disk viewed here is lit dimly by Saturn-shine. This technique, however, requires longer exposure times than those used here to be useful for geologic analysis.

This image has a resolution of 5 km/pixel.