Jets and sources of activity on 67P observed by OSIRIS

Slides:



Advertisements
Similar presentations
Asteroid’s Thermal Models AS3141 Benda Kecil dalam Tata Surya Prodi Astronomi 2007/2008 Budi Dermawan.
Advertisements

Deep Impact Projectsmfa - 1 Deep Impact Projects (2) Mike A’Hearn.
OH Observations of Comets Ellen Howell (Arecibo Observatory) and Amy Lovell (Agnes Scott College)
Comets Astronomy 311 Professor Lee Carkner Lecture 22.
Infrared spectroscopy of Hale-Bopp comet Rassul Karabalin, Ge/Ay 132 Caltech March 17, 2004.
Solar Eclipse Size of Sun, Earth, etc. Lecture 6.
 A star and all of the objects that travel in orbit around it  The area of space that is influenced by the gravity of a star  Our solar system is just.
Adriana V. R. Silva CRAAM/Mackenzie COROT /11/2005.
Asteroids 2867 Steins and 21 Lutetia: results from groundbased observations and from the Rosetta fly-bys S. Fornasier 1,2, M.A. Barucci 1, M. Fulchignoni.
EARLINET and Satellites: Partners for Aerosol Observations Matthias Wiegner Universität München Meteorologisches Institut (Satellites: spaceborne passive.
Folie 1 MUPUS Team Meeting, Graz> I. Pelivan> Thermal Model > Comet Engineering Thermal Model I. Pelivan, E. Kührt.
Chile Sky Background at ESO/la Silla in the Visible and Near IR Leonardo Vanzi -Olivier R. Hainaut European Southern Observatory La Silla - Chile.
Phases of Venus. Share Question How much more solar energy does Venus receive than the Earth, due to the fact that Venus is 0.72 times as far from the.
Alex A. TakedaAug. 18, 2010 Mentor Dr. Alexander Kutyrev.
Imaging Solar Tachocline Using Numerical Simulations and SOHO/MDI Data Junwei Zhao 1, Thomas Hartlep 2, Alexander G. Kosovichev 1, Nagi N. Mansour 2 1.W.W.Hansen.
NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.
The HESSI Imaging Process. How HESSI Images HESSI will make observations of the X-rays and gamma-rays emitted by solar flares in such a way that pictures.
Dokumentname > Dokumentname > B Recent Results of Comet Activity Modeling as input for RPC Plasma Simulations Recent Results of Comet.
Green House Effect and Global Warming. Do you believe that the planet is warming? 1.Yes 2.No.
Micro-structural size properties of Saturn’s rings determined from ultraviolet measurements made by the Cassini Ultraviolet Imaging Spectrograph Todd Bradley.
Rev 51 Enceladus Zeta Orionis Occultation Analysis Status 9 January 2008.
U.A. Dyudina, A.P. Ingersoll, California Institute of Technology Pasadena, CA, Objectives We study lightning on Jupiter using spatially resolved.
Rosetta/OSIRIS observations of gas in the inner coma of 67P
OSIRIS Mars flyby : 3D reconstruction of Phobos and Deimos
Sebastian Höfner, H. Sierks, J.B. Vincent, J. Blum
On the Larger Picture in Cometary Science
Expected dust flux on OSIRIS J. Knollenberg
H. U. Keller, M. Küppers, L. Jorda, P. Gutierrez, S. Hviid, C
OSIRIS Dust Group Studies Overview
Craters on Comets J.-B. Vincent, N. Oklay, S. Marchi, S. Höfner, H. Sierks 33 (6 outlines) -> 27.
Cassini Huygens EECS 823 DIVYA CHALLA.
OSIRIS Full Team Meeting Welcome, Introduction, Agenda
OSIRIS Full Team Meeting -
Outbursts from fractures
C-G: Conundrums and Antagonisms
Environmental Remote Sensing GEOG 2021
Analysis and characterisation of the Aswan *possible* cliff collapse
Astronomy Study Guide Review
Motions of the Moon, Phases and Eclipses (Ch 3)
67P- The bigger Picture H. Uwe Keller.
Fly-By Working Group Meeting
Jean-Baptiste Vincent updated 08 Oct. 2014
J.F. Crifo V.V. Zakharov A.V. Rodionov
Pre-landing Orbiter Observations
Asteroid 4 Vesta observed from OSIRIS-ROSETTA
Seasonal Mass Transport on 67P H. Uwe Keller, S. Mottola, S. Hviid
© University of Wisconsin, CS559 Spring 2004
OSIRIS Science planning
Rosetta ground-based support campaign
S. Besse, M. A’Hearn and the DIXI team
OSIRIS coma dust phase function
33 (6 outlines) -> 27.
ANALYSIS OF SEQUENCE OF IMAGES MTP003/STP004/TRAIL_001 & TRAIL_002
Comet “Anatomy” nucleus (<30km) atmosphere (near sun)
OSIRIS Coma WG report Hans Rickman.
VIRTIS flyby of Steins M-IR Spectral analysis
Changes on the smooth region of Imhotep
Investigation of different flyby geometries for asteroid Steins - Surface area, stereo and phase angle coverage Sofie Spjuth Max-Planck-Institut für Sonnensystemforschung.
Summary of the science planned per mission phase
Photometry of dust grains of comet 67P and connection with nucleus regions G.Cremonese, E.Simioni, R.Ragazzoni, I.Bertini, F.La Forgia, M.Pajola, S.Fornasier,
Remote Detection of Life on Earth ….inferences from EPOXI
Verifying the DCC methodology calibration transfer
The Planets and the Solar System
To Infinity & Beyond….
Section 4 – pg 562 The Outer Planets
Iapetus as measured by Cassini UVIS
On planet earth, we have areas that receive different amounts of the
Our Solar System.
Subsurface properties and early activity of comet 67P/Churyumov-Gerasimenko by Samuel Gulkis, Mark Allen, Paul von Allmen, Gerard Beaudin, Nicolas Biver,
Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun by Alessandra Rotundi, Holger Sierks, Vincenzo Della Corte, Marco Fulle,
Presentation transcript:

Jets and sources of activity on 67P observed by OSIRIS J.-B. Vincent, H. Sierks, L. Lara, P. Gutierez, R. Rodrigo, M. Pajola, N. Oklay, J. Knollenberg, I. Bertini, Z.-Y. Lin, W.-H. Ip, N. Thomas, B. Davidsson, S. Mottola, S. Lowry, S. Fornasier, D. Bodewits, M. Massironi, S. Marchi, S. Hviid, H.U. Keller, S. Besse, L. Jorda, O. Groussin, M. A’Hearn, S. Höfner, C. Snodgrass, and the OSIRIS team OSIRIS team OSIRIS Full Team Meeting 07-10 Oct. 2014

19P/Borelly, Deep Space 1 2001 1P/Halley, GIOTTO 1986 103P/Hartley 2, EPOXI 2010 Comets might be primordial objects at their core, but they have experienced significant surface processing. We need to understand this evolution if we want to link current observations to the origin of the Solar System. How does activity work ? Why some regions are more active than others ? What is the link between coma and surface features ? What is the minimal scale of activity ? Can we identify active areas ? Do we understand which regions will become active in 6 months ? In one year ?

Monitoring 67P's activity with OSIRIS Coma structures in WAC images, July 25-26 2014, 3.67 AU, 3000 km, 300 m/px. At least 3 dust features detected, rotating with the nucleus. Inversion of coma structures links them to bright spots on the nucleus surface, mainly in the transition region between the two lobes. NAC: 50m/px

WAC images, August 05-06 2014, 3.60 AU, 175 km, 12 m/px One large feature visible, focused in a narrow jet some time during the rotation. Combination of projection effect and temporal variation as the illumination conditions are changing with the rotation. Work ongoing on assessing the energy balance and thermal effects. By observing the activity from different angles, we can link dust features in the coma to specific regions on the surface, and morphologic/color information.

Relative brightness Azimuthal profiles at 3km from the nucleus. What fraction of the dust production comes from that particular active source ? We compared brightness in the jet, with average brightness on both sides, ignoring regions affected by ghosts and stray light. "Neck Jet" contributes approximately 10% to the total dust production. The rest of the dust likely comes from smaller jets and/or isotropic emission from the comet's surface.

Linking jets to surface features Red-Green-Blue lines = XYZ axis Black dashed line = jet direction Yellow line = Sun Blue facets = inverted sources Detect jet in images Calculate geometry of observation from shape model + SPICE kernels. Calculate intersection between plane Spacecraft/jet-center and shape model, no constraints on illumination or facet orientation. Repeat for several images => probability map of active sources Use source in forward model, compare output with original images

Modeling Inversion and small scale jets by J.-B. Vincent, COSSIM code 06Aug_04:20 Inversion and small scale jets by J.-B. Vincent, COSSIM code Large scale features modeled by Steve Lowry and Agata Makiela

Increasing resolution… Most jets originate from the neck region and seem correlated to the brightest patches on the surface, as well as outcrops and cliffs. The main jets is actually composed of many small ones, down to a few pixels width. Inversion complicated by the large concavity of this area.

Source(s)? Large cliffs Crack (+ small pits ?) Smooth terrain Outcrops Boulders Small cliffs Pits

Sources ?

Sources ? NAC Twisted jet ! How does it work ?

Activity everywhere Background activity distributed all over the body, what is the main driver ? From August to October: - helio dist went from 3.6 to 3.2 AU, too cold for water ? - sub/Sun latitude went from +45° to +40°

GAS_O1_4

Existing models/Predictions "neck" N activity at perihelion ilumination on landing day, ellipsoid model Vincent et al, A&A, 2013 Inversion of jets from 2003 and 2009 apparitions "most of the activity is located close to the equator and in the southern hemisphere, with only one active region in the north. [...] this region is partially depleted of volatile material, the ice being for instance buried under a deeper layer of dust than in other regions."

Summary 67P is active We see large temporal and spatial variations Stronger activity in the transition region between the two lobes, new regions are waking up everywhere Work ongoing on determining precise source locations, and modeling dust features "Active pits" detected, geomorphological study and continuous monitoring in progress (next talk) Existing models of activity still valid for the jets and their sources