d2jsp
Log InRegister
d2jsp Forums > Off-Topic > General Chat > Science, Technology & Nature > Close Encounter With Comet 67p > May Reveal Origins Of Life On Earth
Prev1242526272851Next
Add Reply New Topic New Poll
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 3 2015 01:02am
catching up with some earlier released pictures:



This single frame Rosetta navigation camera image of Comet 67P/Churyumov-Gerasimenko was taken on 15 June 2015 from a distance of 207 km from the comet centre. The image has a resolution of 17.7 m/pixel and measures 18.1 km across.
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 3 2015 04:45pm
Ice on Comet 67P/Churyumov-Gerasimenko



Released 24/06/2015 3:00 pm
Copyright ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

Examples of six different bright patches identified on the surface of Comet 67P/Churyumov-Gerasimenko in OSIRIS narrow-angle camera images acquired in September 2014. The insets point to the broad regions in which they were discovered (not to specific locations). In total, 120 bright regions, including clusters of bright features, isolated features and individual boulders, were identified in images acquired during September 2014 when the spacecraft was between 20-50 km from the comet centre.

On the left hand side of the image a boulder with icy patches in Hatmehit (top) a cluster of icy features in Imhotep (middle) and a cluster in Khepry (bottom) is presented; on the right hand side a cluster in Anuket (top), a bright feature in Imhotep (middle) and a cluster close to the Khepry-Imhotep boundary (bottom) is shown.

The false colour images are red-green-blue composites assembled from monochrome images taken at different times and have been stretched and slightly saturated to emphasis the contrasts of colour such that dark terrains appear redder and bright regions appear significantly bluer compared with what the human eye would normally see. This imaging technique allows scientists to determine more about the nature of the material; in this case the bluer colour indicates the presence of ice.
Member
Posts: 17,213
Joined: Jan 22 2009
Gold: 0.00
Jul 3 2015 08:58pm
Thanks for the topic been very interesting.
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 3 2015 09:08pm
Quote (cowbooty @ 4 Jul 2015 02:58)
Thanks for the topic been very interesting.



and it will continue to be interesting:

ROSETTA MISSION EXTENDED

23 June 2015
The adventure continues: ESA today confirmed that its Rosetta mission will be extended until the end of September 2016, at which point the spacecraft will most likely be landed on the surface of Comet 67P/Churyumov-Gerasimenko.
Rosetta was launched in 2004 and arrived at the comet in August 2014, where it has been studying the nucleus and its environment as the comet moves along its 6.5-year orbit closer to the Sun. After a detailed survey, Rosetta deployed the lander, Philae, to the surface on 12 November. Philae fell into hibernation after 57 hours of initial scientific operations, but recently awoke and made contact with Rosetta again.
Rosetta’s nominal mission was originally funded until the end of December 2015, but at a meeting today, ESA’s Science Programme Committee has given formal approval to continue the mission for an additional nine months. At that point, as the comet moves far away from the Sun again, there will no longer be enough solar power to run Rosetta’s set of scientific instrumentation efficiently.
“This is fantastic news for science,” says Matt Taylor, ESA’s Rosetta Project Scientist. “We’ll be able to monitor the decline in the comet’s activity as we move away from the Sun again, and we’ll have the opportunity to fly closer to the comet to continue collecting more unique data. By comparing detailed ‘before and after’ data, we’ll have a much better understanding of how comets evolve during their lifetimes.”
Comet on 5 June 2015 – NavCam
Comet 67P/Churyumov-Gerasimenko will make its closest approach to the Sun on 13 August and Rosetta has been watching its activity increase over the last year. Continuing its study of the comet in the year following perihelion will give scientists a fuller picture of how a comet’s activity waxes and wanes along its orbit.
The extra observations collected by Rosetta will also provide additional context for complementary Earth-based observations of the comet. At present, the comet is close to the line-of-sight to the Sun, making ground-based observations difficult.
As the activity diminishes post-perihelion, it should be possible to move the orbiter much closer to the comet’s nucleus again, to make a detailed survey of changes in the comet’s properties during its brief ‘summer’.
In addition, there may be an opportunity to make a definitive visual identification of Philae. Although candidates have been seen in images acquired from a distance of 20 km, images taken from 10 km or less after perihelion could provide the most compelling confirmation.
During the extended mission, the team will use the experience gained in operating Rosetta in the challenging cometary environment to carry out some new and potentially slightly riskier investigations, including flights across the night-side of the comet to observe the plasma, dust, and gas interactions in this region, and to collect dust samples ejected close to the nucleus.
As the comet recedes from the Sun, the solar-powered spacecraft will no longer receive enough sunlight to operate efficiently and safely, equivalent to the situation in June 2011 when the spacecraft was put into hibernation for 31 months for the most distant leg of its journey out towards the orbit of Jupiter.
In addition, Rosetta and the comet will again be close to the Sun as seen from the Earth in October 2016, making operations difficult by then.
However, with Rosetta’s propellant largely depleted by that time, it makes little sense to place the spacecraft in hibernation again.
“This time, as we’re riding along next to the comet, the most logical way to end the mission is to set Rosetta down on the surface,” says Patrick Martin, Rosetta Mission Manager.
“But there is still a lot to do to confirm that this end-of-mission scenario is possible. We’ll first have to see what the status of the spacecraft is after perihelion and how well it is performing close to the comet, and later we will have to try and determine where on the surface we can have a touchdown.”

If this proposed scenario were played out, then the spacecraft would be commanded to spiral down to the comet over a period of about three months.

It is expected that science operations would continue throughout this period and be feasible up to very close to the end of mission, allowing Rosetta’s instruments to gather unique data at unprecedentedly close distances.

Once the orbiter lands on the surface, however, it is highly unlikely to be able to continue operations and relay data back to Earth, bringing to an end one of the most successful space exploration missions of all time.
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 4 2015 10:10am
Active pits on comet



ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA; graphic from J-B Vincent et al (2015)

Left: 18 pits have been identified in high-resolution OSIRIS images of Comet 67P/Churyumov–Gerasimenko’s northern hemisphere. The pits are named after the region they are found in, and some of them are active. The context image was taken on 3 August 2014 by the narrow-angle camera from a distance of 285 km; the image resolution is 5.3 m/pixel.

Middle, top: close-up of the active pit named Seth_01 reveals small jets emanating from the interior walls of the pit. The close-up also shows the complex internal structure of the comet. The image is a section of an OSIRIS wide-angle camera image capture on 20 October 2014 from a distance of 7 km from the comet surface. Seth_01 measures about 220 m across.

Right, top: context image showing fine structure in the comet’s jets as seen from a distance of 28 km from the comet’s surface on 22 November 2014. The image was taken with the OSIRIS wide-angle camera and has a resolution is 2.8 m/pixel. In both images the contrast is deliberately stretched in order to see the details of the activity. The active pits in this study contribute a small fraction of the observed activity.

Left, bottom: how the pits may form through sinkhole collapse. 1. Heat causes subsurface ices to sublimate (blue arrows), forming a cavity (2). When the ceiling becomes too weak to support its own weight, it collapses, creating a deep, circular pit (3, red arrow). Newly exposed material in the pit walls sublimates, accounting for the observed activity (3, blue arrows).
Member
Posts: 7,721
Joined: Oct 11 2008
Gold: 304.00
Jul 4 2015 02:08pm
can you sum up the major points/achievements of this mission?
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 4 2015 07:44pm
for the major targets of the mission you can have a look at the wikipedia article about it
re scientific achievements a summary can only be given once the mission is completed and all the data is analysed
the latter will take till a few months after completion which is now scheduled for late next year
as per technical achievements: getting a probe to accompany a comet and landing a smaller probe on a comet is a first
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 5 2015 09:18am
here a better picture of the active pits:

Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 6 2015 07:05am
more details of some pits:

The evolution of comet pits



Released 01/07/2015 7:00 pm
Copyright ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

Pits Ma’at 1, 2 and 3 on Comet 67P/Churyumov–Gerasimenko show differences in appearance that may reflect their history of activity. While pits 1 and 2 are active, no activity has been observed from pit 3. The young, active pits are particularly steep-sided, whereas pits without any observed activity are shallower and seem to be filled with dust. Middle-aged pits tend to exhibit boulders on their floors from mass-wasting of the sides.

The image was taken with the OSIRIS narrow-angle camera from a distance of 28 km from the comet surface. From left to right the pits measure 125 m, 130 m and 140 m across and are 65 m, 60 m and 50 m deep, respectively.
Member
Posts: 28,331
Joined: Jun 9 2007
Gold: 11,700.00
Jul 9 2015 10:56am
a close-up of some major pits:

Active pits



Released 01/07/2015 7:00 pm
Copyright ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

Active pits detected in the Seth region of Comet 67P/Churyumov-Gerasimenko can be seen in the lower right portion of this OSIRIS wide-angle camera image. The largest, Seth_01, measures 220 m across and 185 m deep. Seth_02 and Seth_03 lie immediately to the left and measure 110 m and 140 m across, respectively.
The contrast of the image has been deliberately stretched to reveal the details of the fine-structured jets against the shadow of the pit, which are interpreted as dusty streams rising from the fractured wall of the pit.
The image was acquired on 20 October 2014 from a distance of 7 km from the surface of the comet.
Go Back To Science, Technology & Nature Topic List
Prev1242526272851Next
Add Reply New Topic New Poll