7 results on '"Dale P. Cruikshank"'
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2. (90377) SEDNA: INVESTIGATION OF SURFACE COMPOSITIONAL VARIATION
- Author
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M. A. Barucci, C. Morea Dalle Ore, Dale P. Cruikshank, C. de Bergh, A. Alvarez-Candal, Christophe Dumas, F. Merlin, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), SETI Institute, NASA Ames Research Center, Moffett Field, and European Southern Observatory
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Physics ,Photometry (optics) ,Solar System ,Spectral signature ,Spitzer Space Telescope ,Space and Planetary Science ,Planet ,Dwarf planet ,Radiative transfer ,Astronomy ,Astronomy and Astrophysics ,Tholin ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
International audience; The dwarf planet (90377) Sedna is one of the most remote solar system objects accessible to investigations. To better constrain its surface composition and to investigate the possible heterogeneity of the surface of Sedna, several observations have been carried out at ESO-VLT with the powerful spectrometer SINFONI observing simultaneously the H and K bands. The analyzed spectra (obtained in 2005, 2007, and 2008) show a non-uniform spectral signature, particularly in the K band. Spectral modeling using the Shkuratov radiative transfer code for surface scattering has been performed using the various sets of data, including previous observations at visible wavelengths and photometry at 3.6 and 4.5 mum by the Spitzer Space Telescope. The visible and near-infrared spectra can be modeled with organic materials (triton and titan tholin), serpentine, and H2O ice in fairly significant amounts, and CH4, N2, and C2H6 in varying trace amounts. One of the spectra obtained in 2005 October shows a different signature in the K band and is best modeled with CH3OH in place of CH4, with reduced amounts of serpentine and with the addition of olivine. The compositional surface heterogeneity can give input on the past history as well clues to the origin of this peculiar, distant object.
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- 2010
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3. Detection of Two Binary Trans-Neptunian Objects, 1997 CQ[TINF]29[/TINF] and 2000 CF[TINF]105[/TINF], with the [ITAL]Hubble Space Telescope[/ITAL]
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John R. Spencer, Marc W. Buie, Stephen C. Tegler, William M. Grundy, W. Romanishin, Keith S. Noll, Dale P. Cruikshank, Robert L. Millis, and Denise C. Stephens
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Physics ,Pluto ,Solar System ,Space and Planetary Science ,Primary (astronomy) ,Hubble space telescope ,Binary number ,Astronomy and Astrophysics ,Trans-Neptunian object ,Astrophysics - Abstract
Images of the trans-Neptunian objects 1997 CQ29 and 2000 CF105 obtained with the Hubble Space Telescope's WFPC2 camera show them to be binary. The two components of 1997 CQ29 were separated in our images by 0.20 arcsec in November 2001 and by 0.33 arcsec in June/July 2002. The corresponding minimum physical distances are 6100 km and 10,200 km. The companion to 2000 CF105 was 0.78 arcsec from the primary, at least 23,400 km. Six other objects in the trans-Neptunian region, including Pluto and its moon Charon, are known to be binaries; 1997 CQ29 and 2000 CF105 are the seventh and eighth known pair. Binarity appears to be a not-uncommon characteristic in this region of the solar system, with detectable companions present in 4% of the objects we have examined.
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- 2002
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4. The Global Color of Pluto from New Horizons
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Silvia Protopapa, Paul M. Schenk, Dennis C. Reuter, Alex Parker, S. Alan Stern, I. Linscott, Kelsi N. Singer, John R. Spencer, Eddie Weigle, Harold A. Weaver, Kimberly Ennico, Cristina M. Dalle Ore, Leslie A. Young, Catherine B. Olkin, Dale P. Cruikshank, Allen W. Lunsford, Marc W. Buie, Bernard Schmitt, Donald E. Jennings, Richard P. Binzel, William M. Grundy, Jason C. Cook, Alissa M. Earle, Ross A. Beyer, and Carly Howett
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Physics ,Pluto ,New horizons ,010504 meteorology & atmospheric sciences ,Space and Planetary Science ,0103 physical sciences ,Astronomy and Astrophysics ,010303 astronomy & astrophysics ,01 natural sciences ,0105 earth and related environmental sciences ,Astrobiology - Published
- 2017
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5. Galileo support observations of Asteroid 951 Gaspra
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Dale P. Cruikshank, David J. Tholen, William K. Hartmann, and Jeffrey D. Goldader
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Physics ,Absolute magnitude ,Photometry (optics) ,Rotation period ,Space and Planetary Science ,Asteroid ,Synodic day ,Astronomy ,Astronomy and Astrophysics ,Astrometry ,Light curve ,Latitude - Abstract
Observations of 951 Gaspra in support of the Galileo spacecraft encounter are reported. Photometric observations of the asteroid yield a synodic rotational period of 7.042 46 and a slope parameter G of 0.285 + or - 0.005. It is inferred from data obtained on May 18, 1990, that the subearth latitude was higher at that time than it was earlier in the opposition. This places a limit on the possible pole orientation of the asteroid. A slope parameter of 0.25 is proposed on the basis of a comparison of the present result for the slope parameter with that of Barucci et al. (1990). A low-quality 0.8-2.5-micron spectrum of 951 Gaspra suggests a high olivine/pyroxene ratio, which is indicative of a source region in the lower mantle of a differentiated asteroid, and similarities to 8 Flora and particularly 15 Eunomia.
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- 1991
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6. Erratum - Infrared Photometry of Nova Serpentis 1978
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Dale P. Cruikshank, E. E. Becklin, R. W. Capps, P. Szkody, and H. M. Dyck
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Physics ,Photometry (astronomy) ,Space and Planetary Science ,Infrared ,Astronomy ,Astronomy and Astrophysics - Published
- 1980
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7. Infrared photometry of Nova Serpentis 1978
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H. M. Dyck, Dale P. Cruikshank, R. W. Capps, P. Szkody, and E. E. Becklin
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Physics ,Infrared astronomy ,Infrared ,Astrophysics::High Energy Astrophysical Phenomena ,Stellar atmosphere ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Wavelength ,Photometry (astronomy) ,Space and Planetary Science ,Thermal radiation ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Cosmic dust - Abstract
Infrared photometry of Nova Ser 1978 was obtained from 36--127 days after the discovery. A prominent dust-shell spectrum was evident in the first observations and its development was followed through maximum infrared light and early decline. The temperature of the dust shell remained between 1100 and 900 K during the observing period. This constant temperature is explained in terms of dust which condenses at a critical radius in continuously outflowing material. It is likely that the dust shell emitting the bulk of the thermal radiation is optically thin at infrared wavelengths. In terms of its dust shell parameters (mass, radius at maximum infrared light and infrared optical thickness) Nova Ser 1978 is very similar to Nova Ser 1970 and Nova Vul 1976.
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- 1979
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