Rosetta: getting close and personal with a comet Matt Taylor, on behalf of the entire Rosetta community
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Rosetta: getting close and personal with a comet
Matt Taylor, on behalf of the entire Rosetta community
A follow up to ESA's first deep space mission, Giotto
Halley, ESA/MPAE, 1986, 1996
Giotto at Halley
Distance 1430 km, resolution 100 m (comet 13 km long)!
Me in 1986
Courtesy of G. Jones, MSSL/UCL
Rosetta
Philae temple of Isis The Rosetta Stone
The combination of the Rosetta Stone and the Philae obelisk were key in deciphering the hieroglyphs and
unlocking the secrets of the civilisation of ancient Egypt.
Fly by’s - 100’s km 10’s km/s
Comet observations Spacecraft visits (imaged...)
• Spacecraft Visits to Comets (imaged) • The Halley Armada
• Giotto, Vega 1 and 2, Suisei, Sakigake
• Deep Space 1 (Borrelly) • Stardust (Wild 2) • Deep Impact (Tempel 1) • EPOXI (Hartley 2) • Rosetta (C-G)
Comet observations Spacecraft visits (imaged...)
• Spacecraft Visits to Comets (imaged) • The Halley Armada
• Giotto, Vega 1 and 2, Suisei, Sakigake
• Deep Space 1 (Borrelly) • Stardust (Wild 2) • Deep Impact (Tempel 1) • EPOXI (Hartley 2) • Rosetta (C-G)
<< 100 km at m/s
Rosetta- 2.8 m x 2.1 m x 2.0 m
32 m Philae - 0.85m x 0.85m (1.3 high and 1.46 m legs)
Rosetta Primary Mission Goals • Catch comet 67P/Churyumov-Gerasimenko in 2014 and accompany it into the interior solar system. • Observe the comet’s nucleus and coma from close range. • Measure the increase in cometary activity during perihelion. • Deploy a robotic lander to make the first controlled landing on a comet nucleus. !
Primary Science Goals • Create a portrait of the comet’s nucleus • Take a complete inventory of the comet’s composition. • Detail the comet’s physical properties • Examine the evolution of activity • Explain the comet’s origin • Create portraits of two asteroids
Rosetta Full suite of insitu and remote sensing instruments
Camera (250–1000nm) Wide-angle (12° FOV) Narrow angle (2.5° FOV) UV spectrometer (70–205nm) VIS and IR mapping spectrometer (250–5000nm) Microwave spectrometer
OSIRIS (H. Sierks, DE) ALICE (A. Stern, US) VIRTIS (F. Cappacioni, IT) MIRO (S. Gulkis, US)
Rosetta
Neutral gas- and ion mass spectrometer Chemical composition of gas in coma Solid mass spectrometer Chemical composition of coma dust Atomic force microscope Shape and size of dust grains
ROSINA (K. Altwegg, CH) COSIMA (M. Hilchenbach, DE) MIDAS (M. Bentley, AT)
Rosetta
Radio transmitter on lander and receiver on orbiter Tomography of nucleus Grain impact analyser and dust collector Rosetta plasma consortium Five plasma instruments Radio science investigation
CONSERT (W. Kofmann, FR) GIADA (A. Rotundi, IT) RPC (Several PI’s) RSI (M. Pätzold, DE)
Rosetta
Philae
Alpha X-ray spectrometer: composition
Six micro-cameras: surface imaging
Radio tomography of nucleus
Evolved gas analyser: organics
Evolved gas analyser: isotopic ratios
Probe on anchor: structure, properties
Imaging system: descent and landing
Magnetometer/plasma monitor
Drill to 20cm: deliver to analysis ovens
Probes comet outer layers
APXS
ÇIVA
CONSERT
COSAC
PTOLEMY
MUPUS
ROLIS
ROMAP
SD2
SESAME
Philae
Rosetta science Comet nuclei Overall, all look different: Different formation or different evolution?
1P/Halley: Highly active, low albedo, relatively little geological information about the surface 19P/Borrelly: Diverse geology, different types of terrain, no ice found on surface! 81P/Wild: Rugged terrain, impact craters ? 9P/Tempel 1: Diverse terrain, primordial layers found?, impact craters ?, very little ice found on surface 103P/Hartley 2: Hyperactive, diverse terrain, extreme shape, ice blocks (cm-dm sized) emitted from nucleus
Rosetta science Comet nuclei Overall, all look different: Different formation or different evolution?
Icy conglomerate Fluffy aggregate
Rubble pile Icy glue
Primodial layers
Nucleus structure
• Cameras will provide images down to 10’s cm resolution: Structural differences will become visible • CONSERT will study the interior structure of the nucleus • Lander will provide ground truth at one position on the nucleus
Rosetta science
Cometary activity - How does the sublimation process work ? How are dust grains accelerated by the gas ?
Rosetta science
• Images and spectra taken of active regions at dm – m scales near nadir (surface) and at the limb (inner coma) Will help understand interaction surface-> coma
• Near-IR and sub-mm spectra will investigate presence of surface ice at high resolution
• ROSINA will measure the gas production and composition throughout the orbit
• GIADA will measure the dust flux and size distribution throughout the orbit Largest sizes may be accessible through imaging
• MIDAS will measure the structure of individual dust particles • COSIMA will measure the composition of individual dust
particles • Lander will provide full information at one point on the surface (if landing on an active area)
How does cometary activity work?
Rosetta science
From Ip and Axford, (1986) STEREO: 2P/Encke, Tail disconnection
• Induced magnetosphere formed by dust - gas emission interaction with solar wind
• Field draping and ion pick up • RPC + ROMAP
Rosetta science
• ROSINA will measure the composition of many species and isotopes, incl. D/H Orders of magnitude more sensitive composition measurement than anything before
• Lander will provide composition and isotope ratios for nucleus material at one point of the surface
• Additional composition information from remote sensing instruments
Composition
Rosetta science
Discovery Perihelion Aphelion Semi-major axis Eccentricity Inclination Orbital period
1969 1.2458 AU 5.6839 AU 3.4648 AU 0.64043 7.0424° 6.45 yr
Klim Churyumov, Jean-Jacques Dordain (ESA), & Svetlana
Gerasimenko at Rosetta launch
Credit: MPS http://www.mps.mpg.de/en/aktuelles/pressenotizen/pressenotiz_20130820.html
Target: 67P/Churyumov-Gerasimenko
Reconstruction of light-curve data rotation rate ~12.7 hours
Lowry et al., 2012
Lamy et al., 2007
Target: 67P/Churyumov-Gerasimenko
Rosetta so far
Launch 2 March 2004 ���First Earth swing-by 4 March 2005���Mars swing-by 25 February 2007���Second Earth swing-by 13 November 2007���Steins fly-by 5 September 2008���Third Earth swing-by 13 November 2009���Lutetia fly-by 10 July 2010���Hibernation Entry 8 June 2011
First Earth !y-by
NavCAM image on March 4, 2005 / ESA
Rosetta so far
Eastwood et al., JGR, 2011
First Earth !y-by Rosetta so far
Rosetta so far
Rosetta at Mars
As seen at 240,000km, one day before fly-by on February 25, 2007 / ESA
Rosetta so far
Near closest approach at 1,000km, February 25, 2007 / ESA
Rosetta so far Rosetta sel"e at Mars
Edberg et al., 2009a+b
Rosetta so far
Near simultaneous observations by Rosetta and Mars Express. Bow shock found closer to planet than expected. 2 point measurements revealed high pressure solar wind pulses to cause asymmetry in the plasma boundaries.
Rosetta at Mars
thanks N. Howes
Asteroid 2867 Šteins Rosetta so far
Fly-by on September 5, 2008
Asteroid 2867 Šteins • Unlocked physical properties of this main-belt asteroid. • Loosely-bound 'rubble pile' whose diamond shape has been honed by
the YORP effect, the modification of rotation rate from IR emission and momentum, redistribute material towards the equator of the object (landslides!)
• This is the first time this effect has been seen in a main-belt asteroid.
5.9 x 4 km, from 800 km at 8.6 km/s H. U. Keller, et al., Science, 2010
ESA ©2008 MPS for OSIRIS Team MPS/UPD/LAM/IAA
ESA ©2009 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA
ESA ©2009 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA
Hurley et al., 2014
Asteroid 21 Lutetia
H. Sierks, et al., Science, 2011
More than 350 craters were identified with diameters between 600 metres and 55 km and depths of up to 10 km, ~3.6 billion years old
121 km x 101 km x 75 km from 3170 km at 15 km/s
Asteroid 21 Lutetia
Movie made from images taken by OSIRIS, released May 30, 2012 / OSIRIS, ESA
Asteroid 21 Lutetia
Fly-by on July 10, 2010
• 21-km diameter crater cluster close to the north pole. • Most of the ejecta from the initial impacts seems to have failed to reach escape velocity and fallen back to the surface. ESA 2010 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA
Copyright ESA 2011 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA and Yuri Beletsky / ESO
And ....sleep.... In the meantime, back on Earth...
http://www.rosetta-campaign.net/
Ground based support and observations of CG 67P
October 2013
ESO/C. Snodgrass (Max Planck Institute for Solar System Research, Germany)
Pro-Am collaborative Astronomy Group Padma A. Yanamandra-Fisher: Flickr, Pinterest, Facebook, twitter
Rosetta Working Group X provides modelling support to the project http://ices.engin.umich.edu/index.php
20 January 2014
Ramp up of outreach campaign - wake up competition
20 January 2014 Hibernation exit.... and an ear worm....
1971 Top of the Pops
Alan Price and Georgie Fame - Rosetta
“Rosetta, are you better? are you well?”
Keep up to date: @ESA_Rosetta
Rosetta blog http://blogs.esa.int/rosetta/
• Nearly 500,000 people watched wakeup • #rosetta and #wakeuprosetta • 32.295 tweets by 18.513 contributors with a reach of 75.11 million people, within 24 hours around the wake up.
Where are we now
Navigation camera - 23 February 2014
Rosetta 2014-2015
ESO- VLT
ESO VLT 28 February 2014
ESO/C. Snodgrass (Max Planck Institute for Solar System Research, Germany) & O. Hainaut (ESO)
Including first light from OSIRIS Wide Angle Camera
around 5 million km from 67P ESA © 2014 MPS for OSIRIS-Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
around 5 million km from 67P ESA © 2014 MPS for OSIRIS-Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA
Including first light from OSIRIS Narrow Angle Camera
M107
VLT image - 7 May 2014
VLT image - 7 May 2014
OSIRIS NAC
27 March 3 April 14 April 17 April 20 April 27 April 4 May
20/01/14-04/05/14: Wake-up and commissioning 05/05/14-02/07/14: NCD phase (‘Near Comet Drift’) 02/07/14-31/07/14: FAT phase (‘Far Approach Trajectory’) 01/08/14-16/08/14: CAT phase (‘Close Approach Trajectory’) 17/08/14-26/08/14: TGM phase (‘Transition to Global Mapping’) 27/08/14-23/09/14: GMP phase (‘Global Mapping Phase’) 24/09/14-25/10/14: COP phase (‘Close Observation Phase’) 26/10/14-11/11/14: Landing preparation and Landing
Rosetta 2014-2015
Separation velocity 0.05 - .5 m/s
at 3 km altitude
Rosetta 2014-2015
Following lander deployment - begin Escort phase of mission
Rosetta 2014-2015
• Navigation relies on navigation camera • ̃ 1.5 hour round trip communication delay • bound orbits only possible at a few 10s km
Rosetta will be the first mission to rendezvous with a
comet, the first mission to escort a comet, travelling at a relative walking pace.
In addition, it will deliver a lander, Philae, to the comet to get
ground truth from insitu measurements.
Will provide the most detailed study of a comet during its closest approach to the Sun
Conclusion
Arrival at comet Lander deployment Perihelion Nominal end-of-mission
Summer 2014 November 2014 August 2015 December 31, 2015
@ESA_Rosetta http://blogs.esa.int/rosetta/
Stay tuned...
END
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