Rosetta: getting close and personal with a comet. Matt Taylor, on behalf of the entire Rosetta community

Transcription

1 Rosetta: getting close and personal with a comet Matt Taylor, on behalf of the entire Rosetta community

2 A follow up to ESA's first deep space mission, Giotto

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4 Giotto at Halley Distance 1430 km, resolution 100 m (comet 13 km long)! Halley, ESA/MPAE, 1986, 1996

5 Me in 1986

6 Courtesy of G. Jones, MSSL/UCL

7 Rosetta The Rosetta Stone Philae temple of Isis 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.

8 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) Fly by s s km 10 s km/s

9 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

10 Rosetta- 2.8 m x 2.1 m x 2.0 m Philae m x 0.85m (1.3 high and 1.46 m legs) 32 m

11 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.!

12 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

13 Rosetta Full suite of insitu and remote sensing instruments

14 Rosetta OSIRIS (H. Sierks, DE) Camera ( nm) Wide-angle (12 FOV) Narrow angle (2.5 FOV) ALICE (A. Stern, US) UV spectrometer (70 205nm) VIRTIS (F. Cappacioni, IT) VIS and IR mapping spectrometer ( nm) MIRO (S. Gulkis, US) Microwave spectrometer

15 Rosetta ROSINA (K. Altwegg, CH) Neutral gas- and ion mass spectrometer Chemical composition of gas in coma COSIMA (M. Hilchenbach, DE) Solid mass spectrometer Chemical composition of coma dust MIDAS (M. Bentley, AT) Atomic force microscope Shape and size of dust grains

16 Rosetta CONSERT (W. Kofmann, FR) Radio transmitter on lander and receiver on orbiter Tomography of nucleus GIADA (A. Rotundi, IT) Grain impact analyser and dust collector RPC (Several PI s) Rosetta plasma consortium Five plasma instruments RSI (M. Pätzold, DE) Radio science investigation

17 Philae

18 Philae APXS ÇIVA CONSERT COSAC PTOLEMY MUPUS ROLIS ROMAP SD2 SESAME 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

19 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

20 Rosetta science Comet nuclei Overall, all look different: Different formation or different evolution? Icy conglomerate Fluffy aggregate Rubble pile Icy glue Primodial layers

21 Rosetta science 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

22 Rosetta science Cometary activity - How does the sublimation process work? How are dust grains accelerated by the gas?

23 Rosetta science How does cometary activity work? 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)

24 Rosetta science Induced magnetosphere formed by dust - gas emission interaction with solar wind Field draping and ion pick up RPC + ROMAP From Ip and Axford, (1986) STEREO: 2P/Encke, Tail disconnection

25 Rosetta science Composition 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

26 Target: 67P/Churyumov-Gerasimenko Klim Churyumov, Jean-Jacques Dordain (ESA), & Svetlana Gerasimenko at Rosetta launch Discovery Perihelion Aphelion Semi-major axis Eccentricity Inclination Orbital period AU AU AU yr Credit: MPS

27 Target: 67P/Churyumov-Gerasimenko Lowry et al., 2012 Reconstruction of light-curve data rotation rate ~12.7 hours Lamy et al., 2007

28 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

29 Rosetta so far First Earth fly-by NavCAM image on March 4, 2005 / ESA

30 Rosetta so far First Earth fly-by Eastwood et al., JGR, 2011

31 Rosetta so far

32 Rosetta so far Rosetta at Mars As seen at 240,000km, one day before fly-by on February 25, 2007 / ESA

33 Rosetta so far Rosetta selfie at Mars Near closest approach at 1,000km, February 25, 2007 / ESA

34 Rosetta so far Rosetta at Mars 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. Edberg et al., 2009a+b

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36 thanks N. Howes

37 Rosetta so far Asteroid 2867 Šteins

38 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 Fly-by on September 5, 2008 ESA 2008 MPS for OSIRIS Team MPS/UPD/LAM/IAA

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40 ESA 2009 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA

41 Hurley et al., 2014 ESA 2009 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA

42 Asteroid 21 Lutetia

43 Asteroid 21 Lutetia 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 H. Sierks, et al., Science, 2011 Movie made from images taken by OSIRIS, released May 30, 2012 / OSIRIS, ESA

44 Asteroid 21 Lutetia ESA 2010 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA 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. Fly-by on July 10, 2010

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46 Copyright ESA 2011 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA and Yuri Beletsky / ESO

47 And...sleep... In the meantime, back on Earth...

48 Ground based support and observations of CG 67P

49 October 2013 ESO/C. Snodgrass (Max Planck Institute for Solar System Research, Germany)

50 Pro-Am collaborative Astronomy Group Padma A. Yanamandra-Fisher: Flickr, Pinterest, Facebook, twitter

51 Rosetta Working Group X provides modelling support to the project

52 Ramp up of outreach campaign - wake up competition 20 January 2014

53 20 January 2014 Hibernation exit... and an ear worm...

54 1971 Top of the Pops Alan Price and Georgie Fame - Rosetta Rosetta, are you better? are you well?

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58 Nearly 500,000 people watched wakeup #rosetta and #wakeuprosetta tweets by contributors with a reach of million people, within 24 hours around the wake up. Keep up to Rosetta blog

59 Where are we now

60 Rosetta Navigation camera - 23 February 2014

61 ESO VLT 28 February 2014 ESO- VLT ESO/C. Snodgrass (Max Planck Institute for Solar System Research, Germany) & O. Hainaut (ESO)

62 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

63 Including first light from OSIRIS Narrow Angle Camera M107 around 5 million km from 67P ESA 2014 MPS for OSIRIS-Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

64 VLT image - 7 May 2014

65 VLT image - 7 May 2014

66 OSIRIS NAC 27 March 3 April 14 April 17 April 20 April 27 April 4 May

67 Rosetta /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

68 Rosetta Separation velocity m/s at 3 km altitude

69 Rosetta Following lander deployment - begin Escort phase of mission Navigation relies on navigation camera 1.5 hour round trip communication delay bound orbits only possible at a few 10s km

70 Conclusion 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

71 Stay Summer 2014 November 2014 August 2015 December 31, 2015 Arrival at comet Lander deployment Perihelion Nominal end-of-mission

72 END