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 Giotto at Halley Distance 1430 km, resolution 100 m (comet 13 km long)! Halley, ESA/MPAE, 1986, 1996 Me in 1986 Courtesy of G. Jones, MSSL/UCL 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. 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 - 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) << 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 Rosetta OSIRIS (H. Sierks, DE) Camera (250–1000nm) 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 (250–5000nm) MIRO (S. Gulkis, US) Microwave spectrometer 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 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 Philae Philae APXS Alpha X-ray spectrometer: composition ÇIVA Six micro-cameras: surface imaging CONSERT Radio tomography of nucleus COSAC Evolved gas analyser: organics PTOLEMY Evolved gas analyser: isotopic ratios MUPUS Probe on anchor: structure, properties ROLIS Imaging system: descent and landing ROMAP Magnetometer/plasma monitor SD2 Drill to 20cm: deliver to analysis ovens SESAME Probes comet outer layers 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 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 Rosetta science Cometary activity - How does the sublimation process work ? How are dust grains accelerated by the gas ? 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) 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 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 Target: 67P/Churyumov-Gerasimenko Klim Churyumov, Jean-Jacques Dordain (ESA), & Svetlana Gerasimenko at Rosetta launch Discovery 1969 Perihelion 1.2458 AU Aphelion 5.6839 AU Semi-major axis 3.4648 AU Eccentricity 0.64043 Inclination 7.0424° Orbital period 6.45 yr http://www.mps.mpg.de/en/aktuelles/pressenotizen/pressenotiz_20130820.html Credit: MPS Target: 67P/Churyumov-Gerasimenko Lowry et al., 2012 Reconstruction of light-curve data rotation rate ~12.7 hours Lamy et al., 2007 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 Rosetta so far First Earth !y-by NavCAM image on March 4, 2005 / ESA Rosetta so far First Earth !y-by Eastwood et al., JGR, 2011 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 Rosetta sel"e at Mars Near closest approach at 1,000km, February 25, 2007 / ESA 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 thanks N. Howes Rosetta so far Asteroid 2867 Šteins 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. H. U. Keller, et al., Science, 2010 5.9 x 4 km, from 800 km at 8.6 km/s Fly-by on September 5, 2008 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 Hurley et al., 2014 ESA ©2009 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA Asteroid 21 Lutetia 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 Asteroid 21 Lutetia • 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 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... Ground based support and observations of CG 67P http://www.rosetta-campaign.net/ 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 Ramp up of outreach campaign - wake up competition 20 January 2014 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?” • 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. Keep up to date: @ESA_Rosetta Rosetta blog http://blogs.esa.int/rosetta/ Where are we now Rosetta 2014-2015 Navigation camera - 23 February 2014 ESO VLT 28 February 2014 ESO- VLT 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 Including first light from OSIRIS Narrow Angle Camera M107 around 5 million