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KAREN J. MEECH February 7, 2019 Astronomer
BIOGRAPHICAL SKETCH – KAREN J. MEECH February 7, 2019 Astronomer Institute for Astronomy Tel: 1-808-956-6828 2680 Woodlawn Drive Fax: 1-808-956-4532 Honolulu, HI 96822-1839 [email protected] PROFESSIONAL PREPARATION Rice University Space Physics B.A. 1981 Massachusetts Institute of Tech. Planetary Astronomy Ph.D. 1987 APPOINTMENTS 2018 – present Graduate Chair 2000 – present Astronomer, Institute for Astronomy, University of Hawaii 1992-2000 Associate Astronomer, Institute for Astronomy, University of Hawaii 1987-1992 Assistant Astronomer, Institute for Astronomy, University of Hawaii 1982-1987 Graduate Research & Teaching Assistant, Massachusetts Inst. Tech. 1981-1982 Research Specialist, AAVSO and Massachusetts Institute of Technology AWARDS 2018 ARCs Scientist of the Year 2015 University of Hawai’i Regent’s Medal for Research Excellence 2013 Director’s Research Excellence Award 2011 NASA Group Achievement Award for the EPOXI Project Team 2011 NASA Group Achievement Award for EPOXI & Stardust-NExT Missions 2009 William Tylor Olcott Distinguished Service Award of the American Association of Variable Star Observers 2006-8 National Academy of Science/Kavli Foundation Fellow 2005 NASA Group Achievement Award for the Stardust Flight Team 1996 Asteroid 4367 named Meech 1994 American Astronomical Society / DPS Harold C. Urey Prize 1988 Annie Jump Cannon Award 1981 Heaps Physics Prize RESEARCH FIELD AND ACTIVITIES • Developed a Discovery mission concept to explore the origin of Earth’s water. • Co-Investigator on the Deep Impact, Stardust-NeXT and EPOXI missions, leading the Earth-based observing campaigns for all three. • Leads the UH Astrobiology Research interdisciplinary program, overseeing ~30 postdocs and coordinating the research with ~20 local faculty and international partners. -
Disintegration of Active Asteroid P/2016 G1 (PANSTARRS) Olivier R
A&A 628, A48 (2019) https://doi.org/10.1051/0004-6361/201935868 Astronomy & © ESO 2019 Astrophysics Disintegration of active asteroid P/2016 G1 (PANSTARRS) Olivier R. Hainaut1, Jan T. Kleyna2, Karen J. Meech2, Mark Boslough3, Marco Micheli4,5, Richard Wainscoat2, Marielle Dela Cruz2, Jacqueline V. Keane2, Devendra K. Sahu6, and Bhuwan C. Bhatt6 1 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany e-mail: [email protected] 2 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 3 University of NM – 1700 Lomas Blvd, NE. Suite 2200, Albuquerque, NM 87131-0001 USA 4 ESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1 00044 Frascati (RM), Italy 5 INAF – Osservatorio Astronomico di Roma, Via Frascati, 33, 00040 Monte Porzio Catone (RM), Italy 6 Indian Institute of Astrophysics, II Block, Koramangala, Bengaluru 560 034, India Received 10 May 2019 / Accepted 26 June 2019 ABSTRACT We report on the catastrophic disintegration of P/2016 G1 (PANSTARRS), an active asteroid, in April 2016. Deep images over three months show that the object is made up of a central concentration of fragments surrounded by an elongated coma, and presents previously unreported sharp arc-like and narrow linear features. The morphology and evolution of these characteristics independently point toward a brief event on 2016 March 6. The arc and the linear feature can be reproduced by large particles on a ring, moving at ∼2:5 m s−1. The expansion of the ring defines a cone with a ∼40◦ half-opening. We propose that the P/2016 G1 was hit by a small object which caused its (partial or total) disruption, and that the ring corresponds to large fragments ejected during the final stages of the crater formation. -
Early Observations of the Interstellar Comet 2I/Borisov
geosciences Article Early Observations of the Interstellar Comet 2I/Borisov Chien-Hsiu Lee NSF’s National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ 85719, USA; [email protected]; Tel.: +1-520-318-8368 Received: 26 November 2019; Accepted: 11 December 2019; Published: 17 December 2019 Abstract: 2I/Borisov is the second ever interstellar object (ISO). It is very different from the first ISO ’Oumuamua by showing cometary activities, and hence provides a unique opportunity to study comets that are formed around other stars. Here we present early imaging and spectroscopic follow-ups to study its properties, which reveal an (up to) 5.9 km comet with an extended coma and a short tail. Our spectroscopic data do not reveal any emission lines between 4000–9000 Angstrom; nevertheless, we are able to put an upper limit on the flux of the C2 emission line, suggesting modest cometary activities at early epochs. These properties are similar to comets in the solar system, and suggest that 2I/Borisov—while from another star—is not too different from its solar siblings. Keywords: comets: general; comets: individual (2I/Borisov); solar system: formation 1. Introduction 2I/Borisov was first seen by Gennady Borisov on 30 August 2019. As more observations were conducted in the next few days, there was growing evidence that this might be an interstellar object (ISO), especially its large orbital eccentricity. However, the first astrometric measurements do not have enough timespan and are not of same quality, hence the high eccentricity is yet to be confirmed. This had all changed by 11 September; where more than 100 astrometric measurements over 12 days, Ref [1] pinned down the orbit elements of 2I/Borisov, with an eccentricity of 3.15 ± 0.13, hence confirming the interstellar nature. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
An Anisotropic Distribution of Spin Vectors in Asteroid Families
Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes. -
Elements of Astronomy
^ ELEMENTS ASTRONOMY: DESIGNED AS A TEXT-BOOK uabemws, Btminwcus, anb families. BY Rev. JOHN DAVIS, A.M. FORMERLY PROFESSOR OF MATHEMATICS AND ASTRONOMY IN ALLEGHENY CITY COLLEGE, AND LATE PRINCIPAL OF THE ACADEMY OF SCIENCE, ALLEGHENY CITY, PA. PHILADELPHIA: PRINTED BY SHERMAN & CO.^ S. W. COB. OF SEVENTH AND CHERRY STREETS. 1868. Entered, according to Act of Congress, in the year 1867, by JOHN DAVIS, in the Clerk's OlBce of the District Court of the United States for the Western District of Pennsylvania. STEREOTYPED BY MACKELLAR, SMITHS & JORDAN, PHILADELPHIA. CAXTON PRESS OF SHERMAN & CO., PHILADELPHIA- PREFACE. This work is designed to fill a vacuum in academies, seminaries, and families. With the advancement of science there should be a corresponding advancement in the facilities for acquiring a knowledge of it. To economize time and expense in this department is of as much importance to the student as frugality and in- dustry are to the success of the manufacturer or the mechanic. Impressed with the importance of these facts, and having a desire to aid in the general diffusion of useful knowledge by giving them some practical form, this work has been prepared. Its language is level to the comprehension of the youthful mind, and by an easy and familiar method it illustrates and explains all of the principal topics that are contained in the science of astronomy. It treats first of the sun and those heavenly bodies with which we are by observation most familiar, and advances consecutively in the investigation of other worlds and systems which the telescope has revealed to our view. -
Trojans Swarms
Asteroids, Trojans and Transneptunians Sonia Fornasier LESIA-Obs. de Paris/Univ Paris Diderot The solar system debris disks - Small bodies: Preserve evidence of conditions early in solar system history - TNO: cold and relatively unprocessed - They trace Solar System formation and evolution - Delivery of water and organics to the Earth 2 …and exo-systems disk debris ~400 long, highly elongated 1I/2017 U1 'Oumuamua • First interstellar asteroid discovered on 18 Oct. 2017 (William 2017) • Q=0.254 AU, e=1.197, i=122.6 °, v∞ = 25 km/s • very elongated shape (10:1 axis ratio and a mean radius of 102±4 m, assuming an albedo of 0.04, Meech et al., 2017) • No cometary activity, red spectrum similar to D-type (Jewitt et al., 2017) More than 700000 asteroids discovered Crust Wide diversity of composition, shape, structures mantle Pristine (D, C) silicaceous (S, A) Igneous (E,V) core S E C Rosetta (ESA) ρ=2.7 S: silicaceous asteroids, Steins: differentiated objet similar to the ordinary enstatite rich chondrite (space Vesta: differentiated Dawn (NASA) V weathering effects) object with internal structure (Density 3,5) Itokawa -parent body of HED achondrite Mathilde ρ=1.95 ρ=1.3 S C/D: carbonaceous and organic material, hydrated silicates ( liquid water in the past), small M-type: high density, densities, high porosity Rubble pile exposed nickel-iron Similarities with carbonaceus structure core of an early planet chondrites Shepard et al., 2017 Focus on primitive asteroids, TNOs The water problematic and evidence of its past and current presence in the main belt (aqueous alteration, ice) Families studies: the Themis/Beagle case Space weathering issues The Trojans population TNOs/Centaurs The water problematic in Asteroids ● Nebular snowline ● A lot of mass in H2O ● Big effect on accretion where condenses Dodson-Robinson et al. -
A Low Density of 0.8 G Cm-3 for the Trojan Binary Asteroid 617 Patroclus
Publisher: NPG; Journal: Nature:Nature; Article Type: Physics letter DOI: 10.1038/nature04350 A low density of 0.8 g cm−3 for the Trojan binary asteroid 617 Patroclus Franck Marchis1, Daniel Hestroffer2, Pascal Descamps2, Jérôme Berthier2, Antonin H. Bouchez3, Randall D. Campbell3, Jason C. Y. Chin3, Marcos A. van Dam3, Scott K. Hartman3, Erik M. Johansson3, Robert E. Lafon3, David Le Mignant3, Imke de Pater1, Paul J. Stomski3, Doug M. Summers3, Frederic Vachier2, Peter L. Wizinovich3 & Michael H. Wong1 1Department of Astronomy, University of California, 601 Campbell Hall, Berkeley, California 94720, USA. 2Institut de Mécanique Céleste et de Calculs des Éphémérides, UMR CNRS 8028, Observatoire de Paris, 77 Avenue Denfert-Rochereau, F-75014 Paris, France. 3W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, Hawaii 96743, USA. The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°). The asteroid 617 Patroclus is the only known binary Trojan1. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system’s centre of mass, describing a roughly circular orbit. Using this orbital information, combined with thermal measurements to estimate +0.2 −3 the size of the components, we derive a very low density of 0.8 −0.1 g cm . The components of 617 Patroclus are therefore very porous or composed mostly of water ice, suggesting that they could have been formed in the outer part of the Solar System2. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
IMPLICATIONS of ASTEROIDAL SATELLITES. W.J. Merline1 and C.R
64th Annual Meteoritical Society Meeting (2001) 5457.pdf IMPLICATIONS OF ASTEROIDAL SATELLITES. W.J. Merline1 and C.R. Chapman2, 1Southwest Research Institute ([email protected]), 2Southwest Research Institute ([email protected]) There has been a recent revolution in asteroid astron- strange objects like the highly elongated metallic ob- omy that may have important implications for meteor- ject Kleopatra and the recently discovered distant sat- ite parent bodies. In short, in the last 8 years, it has ellite of a Kuiper Belt Object, could be a remnant from been found that numerous asteroids are double bodies accretionary processes. or have small satellites orbiting about them. The first one to be discovered (the 1.8 km moonlet found by the In thinking about where meteorites come from, it Galileo spacecraft to be orbiting around 31 km-sized would help parent-body modelers to have a mental Ida during a 1993 flyby) could have been a fluke, since framework that includes the kinds of configurations the accepted theoretical perspective at the time was now being discovered and the potential processes these that such satellites would be very rare or absent. How- bodies have been through before delivering meteorites ever, we now know that at least several percent of to our collections. Certainly there are implications main-belt asteroids are binaries and that a large per- from the existence of asteroidal satellites for the char- centage of Earth-approaching asteroids are binaries. acter of rubble piles, exposure ages of asteroidal rocks, and so on. The existence of double impact craters on It is not known with certainty how these satellites are the Earth and other planets may now have a more natu- created, but it is likely to be due to several different ral explanation. -
The Veritas and Themis Asteroid Families: 5-14Μm Spectra with The
Icarus 269 (2016) 62–74 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Veritas and Themis asteroid families: 5–14 μm spectra with the Spitzer Space Telescope Zoe A. Landsman a,∗, Javier Licandro b,c, Humberto Campins a, Julie Ziffer d, Mario de Prá e, Dale P. Cruikshank f a Department of Physics, University of Central Florida, 4111 Libra Drive, PS 430, Orlando, FL 32826, United States b Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38205, La Laguna, Tenerife, Spain c Departamento de Astrofísica, Universidad de La Laguna, E-38205, La Laguna, Tenerife, Spain d Department of Physics, University of Southern Maine, 96 Falmouth St, Portland, ME 04103, United States e Observatório Nacional, R. General José Cristino, 77 - Imperial de São Cristóvão, Rio de Janeiro, RJ 20921-400, Brazil f NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035, United States article info abstract Article history: Spectroscopic investigations of primitive asteroid families constrain family evolution and composition and Received 18 October 2015 conditions in the solar nebula, and reveal information about past and present distributions of volatiles in Revised 30 December 2015 the solar system. Visible and near-infrared studies of primitive asteroid families have shown spectral di- Accepted 8 January 2016 versity between and within families. Here, we aim to better understand the composition and physical Available online 14 January 2016 properties of two primitive families with vastly different ages: ancient Themis (∼2.5 Gyr) and young Ver- Keywords: itas (∼8 Myr). We analyzed the 5 – 14 μm Spitzer Space Telescope spectra of 11 Themis-family asteroids, Asteroids including eight previously studied by Licandro et al. -
Observing Water in Our Solar System
Observing water in our Solar System Colin Snodgrass Ice in our Solar System www.nightsky.ie www.nightsky.ie 250 K 150 K 50 K Equilibrium temperature drops with distance ( d-½ ) Present day snow line is at ~2.7 AU from Sun, in asteroid belt. Ice exists on surfaces in Kuiper Belt. In inner solar system, sublimation drives cometary activity. Kuiper Belt Objects – Haumea Spectroscopy of KBOs, particularly in the NIR, reveals differences in their surface ices. Haumea ‘family’ have spectra that match almost pure water ice. Remains from a collision. We used the VLT+Hawk-I to identify ices on potential family members using photometry. Snodgrass et al 2010, Carry et al (submitted) Further Family Members Ragozzine & Brown (2007, AJ 134, p2160) published a list of further family member candidates selected on dynamical grounds. The orbits in the TN region (and interactions with resonances) make this difficult to do. Need to confirm that they share the same water ice surface to be true family members. However, most are too faint for the NIR spectroscopy that can unambiguously detect water ice. Water Ice Detection We use HAWK-I at the VLT to perform J and CH4 band photometry, using the CH4 band as a narrower H band. We confirm that our measurements of (J-Hs) are sensitive to water ice. We measured this colour for 18 objects. 6 are objects previously claimed as family members - they have strongly negative (J-Hs). 2 other objects are confirmed as family members, 2003 SQ317 and 2005 CB79. The remaining 10 (including non-candidate Eris, observed for comparison) have positive values and we rule out water ice surfaces.