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Published October 20, 2007 | Published + Submitted
Journal Article Open

The Dust, Planetesimals, and Planets of HD 38529


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).

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.

Attached Files

Published - Moro-Martín_2007_ApJ_668_1165.pdf

Submitted - 0706.3368.pdf


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August 22, 2023
October 26, 2023