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Title: ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK

Abstract

We present resolved images of the HR 4796A debris disk using the Magellan adaptive optics system paired with Clio-2 and VisAO. We detect the disk at 0.77 μm, 0.91 μm, 0.99 μm, 2.15 μm, 3.1 μm, 3.3 μm, and 3.8 μm. We find that the deprojected center of the ring is offset from the star by 4.76 ± 1.6 AU and that the deprojected eccentricity is 0.06 ± 0.02, in general agreement with previous studies. We find that the average width of the ring is 14{sub −2}{sup +3}% (11.1{sub −1.6}{sup +2.4} AU), also comparable to previous measurements. Combining our new scattered light data with archival Hubble Space Telescope images at ∼0.5-2 μm, along with previously unpublished Spitzer/MIPS thermal emission data and all other literature thermal data, we set out to constrain the chemical composition of the dust grains. After testing 19 individual root compositions and more than 8400 unique mixtures of these compositions, we find that good fits to the scattered light alone and thermal emission alone are discrepant, suggesting that caution should be exercised if fitting to only one or the other. When we fit to both data sets simultaneously, we find that silicates and organics are generally the most favored, while large abundances of watermore » ice are usually not favored. These results suggest the HR 4796A dust grains are similar to interstellar dust and solar system comets, though improved modeling is necessary to place better constraints on the exact chemical composition of the dust.« less

Authors:
;  [1];  [2]; ;  [3]; ; ; ; ; ; ; ; ;  [4]; ; ; ; ; ;  [5]
  1. Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015 (United States)
  2. NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics Laboratory, Code 667, Greenbelt, MD 20771 (United States)
  3. Space Telescope Science Institute, Baltimore, MD 21218 (United States)
  4. Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)
  5. INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125, Firenze (Italy)
Publication Date:
OSTI Identifier:
22364648
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 798; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CHEMICAL COMPOSITION; COMETS; COMPARATIVE EVALUATIONS; COMPUTERIZED SIMULATION; COSMIC DUST; ICE; IMAGES; INTERSTELLAR SPACE; MIXTURES; MORPHOLOGY; OPTICS; SILICATES; SOLAR SYSTEM; STARS; TELESCOPES; VISIBLE RADIATION

Citation Formats

Rodigas, Timothy J., Weinberger, Alycia, Stark, Christopher C., Debes, John H., Chen, Christine, Hinz, Philip M., Close, Laird, Smith, Paul S., Males, Jared R., Skemer, Andrew J., Follette, Katherine B., Morzinski, Katie, Wu, Ya-Lin, Schneider, Glenn, Puglisi, Alfio, Briguglio, Runa, Esposito, Simone, Pinna, Enrico, Riccardi, Armando, and Xompero, Marco, E-mail: trodigas@carnegiescience.edu. ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK. United States: N. p., 2015. Web. doi:10.1088/0004-637X/798/2/96.
Rodigas, Timothy J., Weinberger, Alycia, Stark, Christopher C., Debes, John H., Chen, Christine, Hinz, Philip M., Close, Laird, Smith, Paul S., Males, Jared R., Skemer, Andrew J., Follette, Katherine B., Morzinski, Katie, Wu, Ya-Lin, Schneider, Glenn, Puglisi, Alfio, Briguglio, Runa, Esposito, Simone, Pinna, Enrico, Riccardi, Armando, & Xompero, Marco, E-mail: trodigas@carnegiescience.edu. ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK. United States. doi:10.1088/0004-637X/798/2/96.
Rodigas, Timothy J., Weinberger, Alycia, Stark, Christopher C., Debes, John H., Chen, Christine, Hinz, Philip M., Close, Laird, Smith, Paul S., Males, Jared R., Skemer, Andrew J., Follette, Katherine B., Morzinski, Katie, Wu, Ya-Lin, Schneider, Glenn, Puglisi, Alfio, Briguglio, Runa, Esposito, Simone, Pinna, Enrico, Riccardi, Armando, and Xompero, Marco, E-mail: trodigas@carnegiescience.edu. Sat . "ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK". United States. doi:10.1088/0004-637X/798/2/96.
@article{osti_22364648,
title = {ON THE MORPHOLOGY AND CHEMICAL COMPOSITION OF THE HR 4796A DEBRIS DISK},
author = {Rodigas, Timothy J. and Weinberger, Alycia and Stark, Christopher C. and Debes, John H. and Chen, Christine and Hinz, Philip M. and Close, Laird and Smith, Paul S. and Males, Jared R. and Skemer, Andrew J. and Follette, Katherine B. and Morzinski, Katie and Wu, Ya-Lin and Schneider, Glenn and Puglisi, Alfio and Briguglio, Runa and Esposito, Simone and Pinna, Enrico and Riccardi, Armando and Xompero, Marco, E-mail: trodigas@carnegiescience.edu},
abstractNote = {We present resolved images of the HR 4796A debris disk using the Magellan adaptive optics system paired with Clio-2 and VisAO. We detect the disk at 0.77 μm, 0.91 μm, 0.99 μm, 2.15 μm, 3.1 μm, 3.3 μm, and 3.8 μm. We find that the deprojected center of the ring is offset from the star by 4.76 ± 1.6 AU and that the deprojected eccentricity is 0.06 ± 0.02, in general agreement with previous studies. We find that the average width of the ring is 14{sub −2}{sup +3}% (11.1{sub −1.6}{sup +2.4} AU), also comparable to previous measurements. Combining our new scattered light data with archival Hubble Space Telescope images at ∼0.5-2 μm, along with previously unpublished Spitzer/MIPS thermal emission data and all other literature thermal data, we set out to constrain the chemical composition of the dust grains. After testing 19 individual root compositions and more than 8400 unique mixtures of these compositions, we find that good fits to the scattered light alone and thermal emission alone are discrepant, suggesting that caution should be exercised if fitting to only one or the other. When we fit to both data sets simultaneously, we find that silicates and organics are generally the most favored, while large abundances of water ice are usually not favored. These results suggest the HR 4796A dust grains are similar to interstellar dust and solar system comets, though improved modeling is necessary to place better constraints on the exact chemical composition of the dust.},
doi = {10.1088/0004-637X/798/2/96},
journal = {Astrophysical Journal},
number = 2,
volume = 798,
place = {United States},
year = {Sat Jan 10 00:00:00 EST 2015},
month = {Sat Jan 10 00:00:00 EST 2015}
}