Nearby Debris Disk Systems with High Fractional Luminosity Reconsidered

By A. Moór, P. Ábrahám, A. Derekas, C. Kiss, L. Kiss, D. Apai, C. Grady, Th. Henning. 2006

188 citations recorded by the source corpus.

By searching the IRAS and ISO databases, we compiled a list of 60 debris disks that exhibit the highest fractional luminosity values (fd > 10-4) in the vicinity of the Sun (d < 120 pc). Eleven out of these 60 systems are new discoveries. Special care was taken to exclude bogus disks from the sample. We computed the fractional luminosity values using available IRAS, ISO, and Spitzer data and analyzed the Galactic space velocities of the objects. The results revealed that stars with disks of high fractional luminosity often belong to young stellar kinematic groups, providing an opportunity to obtain improved age estimates for these systems. We found that practically all disks with fd > 5 × 10-4 are younger than 100 Myr. The distribution of the disks in the fractional luminosity versus age diagram indicates that (1) the number of old systems with high fd is lower than was claimed before, (2) there exist many relatively young disks of moderate fractional luminosity, and (3) comparing the observations with a current theoretical model of debris disk evolution, a general good agreement could be found.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/db9f182ff9f4afdeb4b71ef3d0925742f61b2847

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In Astronomy and Astrophysics

1. Eric Mamajek
2. K. Luhman
3. L. Hillenbrand
4. B. Bowler
5. C. Bell
6. Michael C. Liu
7. S. Kenyon
8. D. Lafrèniere

In Instrumentation

1. Eric Mamajek
2. L. Hillenbrand
3. C. Bell
4. K. Luhman
5. S. Kenyon
6. B. Bromley
7. M. C. Wyatt
8. R. Doyon

Citations in the corpus

• BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS (2012, background): “…all radial velocity measurements from the previous studies of Hawley et al. (1996); Montes et al. (2001); Gizis et al. (2002); Torres et al. (2006); Moór et al. (2006); Lépine & Simon (2009); Schlieder et al. (2010); Looper et al. (2010); Kiss et al. (2011); Rodriguez et al. (2011); Siebert et al.…”
• 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).”
• A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, background): “4 Columba HD 15115 was previously believed to be a member of the BPMG (see e.g. Moór et al. 2006), however Malo et al. (2013) suggests that it is more likely to be a member of Columba (Pv+π = 87 per cent) and therefore we retain this as a member of Columba for the age determination.”
• Debris Disks around Sun-like Stars (2007, methodology): “Nevertheless, this system may be useful in helping to define the exact border of the distribution discussed by Moór et al. (2006).”
• Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs (2006, methodology): “Most recently, Moór et al. (2006) compiled a list of 60 debris disks with high fractional dust luminosity, > 10 4, and within 120 pc of Earth by searching the IRAS and ISO databases.”
• 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).”
• 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).”
• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “…(ISO), and Spitzer Space Telescope have revealed substantial mid-infrared (mid-IR) excesses associated with hundreds of normal mainsequence stars (e.g., Backman & Paresce1993; Habing et al. 2001; Zuckerman 2001; Rieke et al. 2005; Bryden et al. 2006;Moór et al. 2006; Rhee et al. 2007a).”
• Debris disks as signposts of terrestrial planet formation (2011, background): “…broadly consistent with the fluxes detected around solar-type stars with observed excesses at 24 and 70 μm (Habing et al. 2001; Beichman et al. 2006; Moór et al. 2006; Trilling et al. 2008; Hillenbrand et al. 2008; Carpenter et al. 2009; Gáspár et al. 2009), although our stable simulations yield…”
• Long-Term Collisional Evolution of Debris Disks (2007, unknown): “5 < α < 1.0, Spangler et al. (2001) reportα ≈ 1.8, and Greaves (2005) and Moór et al. (2006) deriveα ≈ 1.0.”