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The Dust, Planetesimals, and Planets of HD 38529

Moro-Martín, Amaya and Malhotra, Renu and Carpenter, John M. and Hillenbrand, Lynne A. and Wolf, Sebastian and Meyer, Michael R. and Hollenbach, David and Najita, Joan and Henning, Thomas (2007) The Dust, Planetesimals, and Planets of HD 38529. Astrophysical Journal, 668 (2). pp. 1165-1173. ISSN 0004-637X. doi:10.1086/521093.

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HD 38529 is a post-main-sequence G8 III/IV star (3.5 Gyr old) with a planetary system consisting of at least two planets having M sin i of 0.8 and 12.2 M_(Jup), semimajor axes of 0.13 and 3.74 AU, and eccentricities of 0.25 and 0.35, respectively. Spitzer observations show that HD 38529 has an excess emission above the stellar photosphere, with a signal-to-noise ratio (S/N) at 70 μm of 4.7, a small excess at 33 μm (S/N = 2.6), and no excess <30 μm. We discuss the distribution of the potential dust-producing planetesimals from the study of the dynamical perturbations of the two known planets, considering in particular the effect of secular resonances. We identify three dynamically stable niches at 0.4-0.8, 20-50, and beyond 60 AU. We model the spectral energy distribution (SED) of HD 38529 to find out which of these niches show signs of harboring dust-producing planetesimals. The secular analysis, together with the SED modeling results, suggest that the planetesimals responsible for most of the dust emission are likely located within 20-50 AU, a configuration that resembles that of the Jovian planets + Kuiper Belt in our solar system. Finally, we place upper limits (8 × 10^(-6) lunar masses of 10 μm particles) to the amount of dust that could be located in the dynamically stable region that exists between the two planets (0.25-0.75 AU).

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Moro-Martín, Amaya0000-0001-9504-8426
Malhotra, Renu0000-0002-1226-3305
Carpenter, John M.0000-0003-2251-0602
Meyer, Michael R.0000-0003-1227-3084
Additional Information:© 2007 American Astronomical Society. Received 2007 February 3. Accepted 2007 June 22. We thank the rest of the FEPS team members, colleagues at the Spitzer Science Center, and members of all the Spitzer instrument teams for advice and support. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contrast 1407. A. M.-M. is under contract with the Jet Propulsion Laboratory (JPL), funded by NASA through the Michelson Fellowship Program. JPL is managed for NASA by the California Institute of Technology. A. M.-M. is also supported by the Lyman Spitzer Fellowship at Princeton University. R. M. and M. R. M. are supported in part through the LAPLACE node of NASA's Astrobiology Institute. R. M. also acknowledges support from NASA's Origins of Solar Systems research program. S. W. was supported through DFG Emmy Noether grants WO 875/2-1 and WO 875/2-2. FEPS is pleased to acknowledge support from NASA contracts 1224768 and 1224566, administered through JPL.
Funding AgencyGrant Number
NASA Michelson FellowshipUNSPECIFIED
Princeton UniversityUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)WO 875/2-1
Deutsche Forschungsgemeinschaft (DFG)WO 875/2-2
Subject Keywords:circumstellar matter; infrared: stars; Kuiper Belt; planetary systems; stars: individual (HD 38529)
Issue or Number:2
Record Number:CaltechAUTHORS:20170808-094604378
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Official Citation:Amaya Moro-Martín et al 2007 ApJ 668 1165
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:79921
Deposited By: Ruth Sustaita
Deposited On:09 Aug 2017 19:30
Last Modified:15 Nov 2021 17:51

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