Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs

By J. H. Rhee, Inseok Song, B. Zuckerman, M. McElwain. 2006

207 citations recorded by the source corpus.

Dusty debris disks around main-sequence stars are signposts for the existence of planetesimals and exoplanets. From cross-correlating Hipparcos stars with the IRAS catalogs, we identify 146 stars within 120 pc of Earth that show excess emission at 60 μm. This search took special precautions to avoid false positives. Our sample is reasonably well distributed from late B to early K-type stars, but it contains very few later type stars. Even though IRAS flew more than 20 years ago and many astronomers have cross-correlated its catalogs with stellar catalogs, we were still able to newly identify debris disks at as many as 33 main-sequence stars; of these, 32 are within 100 pc of Earth. The power of an all-sky survey satellite like IRAS is evident when comparing our 33 new debris disks with the total of only 22 dusty debris disk stars first detected with the more sensitive, but pointed, satellite ISO. Our investigation focuses on the mass, dimensions, and evolution of dusty debris disks.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/69b5d9c8720b7b85c9cea0acf3d14387d76b31b9

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In Astronomy and Astrophysics

1. Eric Mamajek
2. L. Hillenbrand
3. K. Luhman
4. B. Zuckerman
5. S. Kenyon
6. M. C. Wyatt
7. B. Bromley
8. Inseok Song

Citations in the corpus

• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “The predicted rate of decline, t n with n 0:6Y0:8, is close to the observed rate (n 0:5Y1; Greaves & Wyatt 2003; Rieke et al. 2005; Rhee et al. 2007a).”
• FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS (2008, background): “…relationship between debris dust and planetary systems has moti- vated many studies to investigate the frequency and properties of debris disks (Aumann & Probst 1991; Mannings & Barlow 1998; Moór et al. 2006; Rhee et al. 2007, see also Lagrange, Backman, & Artymo 2000 and references therein).”
• NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, unknown): “…a flux-limited survey could partially account for this apparent difference in disk frequency and disk lifetime; debris disks around K and M dwarfs are thought to be relatively colder and fainter than around solartype stars, due to the lower stellar luminosities (Rhee et al. 2007; Zuckerman 2001).”
• NEAR-INFRARED SPECTROSCOPY OF THE EXTRASOLAR PLANET HR 8799 b (2010, unknown): “…implying an architecture analogous to our Solar System with giant planets surrounded by “exo-asteroid” and “exo-Kuiper” belts (Sadakane & Nishida 1986; Zuckerman & Song 2004; Moór et al. 2006; Williams & Andrews 2006; Rhee et al. 2007; Chen et al. 2009; Su et al. 2009; Reidemeister et al. 2009).”
• The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, unknown): “Source of literature isochrone ages Reference Number of Stars Gerbaldi et al. (1999) 4 Janson et al. (2011) 1 Laureijs et al. (2002) 1 Paunzen (1997) 3 Rhee et al. (2007) 25 Rieke et al. (2005) 8 Song et al. (2001) 6 Su et al. (2006) 1 Tetzlaff et al. (2010) 12 Westin (1985) 3 diagram (Fig.”
• Debris Disks around Sun-like Stars (2007, methodology): “…at wavelengths of 10–100 m. Data from the Infrared Astronomical Satellite (IRAS ) and Infrared Space Observatory (ISO) were used to identify and characterize debris disks (e.g., Aumann et al. 1984; Decin et al. 2000; Spangler et al. 2001; Habing et al. 2001; Decin et al. 2003; Rhee et al. 2007).”
• THE TUCANA/HOROLOGIUM, COLUMBA, AB DORADUS, AND ARGUS ASSOCIATIONS: NEW MEMBERS AND DUSTY DEBRIS DISKS (2011, background): “Almost all of these excesses are measured most convincingly at 60 microns wavelength (Moor et al 2006, Rhee et al 2007a and references therein), although occasionally instead at 25 microns (Rhee et al 2007b and Melis et al 2010 and references therein).”
• Steady State Evolution of Debris Disks around A Stars (2007, background): “…& Williams (2005) found the mass of the detected disks falls off ∝ t−1, and the upper limit in 24 µm of the A star disks was found to fall off ∝ t−1 (Rieke et al. 2005), while disk mass from far-IR statistics was inferred to be relatively age independent in the range 30-1000 Myr (Rhee et al. 2007).”
• ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS (2010, background): “Both IRAS (Rhee et al 2007) and Spitzer (Su et al 2006; Trilling et al 2008) surveys of intermediate mass stars (primarily A- and F-type) indicate that the fraction of such stars with detectable debris disks declines with stellar age.”