Incidence and survival of remnant disks around main-sequence stars

By H. Habing, C. Dominik, M. J. Muizon, R. Laureijs, M. Kessler, K. Leech, L. Metcalfe, A. Salama, R. Siebenmorgen, N. Trams and 1 more. 2000

165 citations recorded by the source corpus.

We present photometric ISO 60 and 170 um measurements, complemented by some IRAS data at 60 ${\mu\textrm{m}}$, of a sample of 84 nearby main-sequence stars of spectral class A, F, G and K in order to determine the incidence of dust disks around such main-sequence stars. Fifty stars were detected at 60 ${\mu\textrm{m}}$; 36 of these emit a flux expected from their photosphere while 14 emit significantly more. The excess emission we attribute to a circumstellar disk like the ones around Vega and β Pictoris. Thirty four stars were not detected at all; the expected photospheric flux, however, is so close to the detection limit that the stars cannot have an excess stronger than the photospheric flux density at 60 ${\mu\textrm{m}}$. Of the stars younger than 400 Myr one in two has a disk; for the older stars this is true for only one in ten. We conclude that most stars arrive on the main sequence surrounded by a disk; this disk then decays in about 400 Myr. Because (i) the dust particles disappear and must be replenished on a much shorter time scale and (ii) the collision of planetesimals is a good source of new dust, we suggest that the rapid decay of the disks is caused by the destruction and escape of planetesimals. We suggest that the dissipation of the disk is related to the heavy bombardment phase in our Solar System. Whether all stars arrive on the main sequence surrounded by a disk cannot be established: some very young stars do not have a disk. And not all stars destroy their disk in a similar way: some stars as old as the Sun still have significant disks.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e5aad15c383b66886982c60b77040deecd3d3beb

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Citations in the corpus

Decay of Planetary Debris Disks (2005, background): “Such studies suggest an anticorrelation between stellar age and the magnitude of infrared excess, with timescales for the decline of the excess emission of hundreds of millions of years (e.g., Habing et al. 2001).”
New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets (2006, background): “In contrast with a simple reading of equation (3), the Habing et al. (2001) models have Ldust/L more or less directly proportional to Fdust/F for stars of type G and earlier.”
A Survey and Analysis of Spitzer Infrared Spectrograph Spectra of T Tauri Stars in Taurus (2006, background): “A dust mass of a few times 10 4 lunar masses is comparable to that found around debris disks (Habing et al. 2001), although closer to the lower mass values.”
Dust Dynamics, Surface Brightness Profiles, and Thermal Spectra of Debris Disks: The Case of AU Microscopii (2005, background): “Most debris disks are inferred to exist from measurements of infrared excesses (e.g., Aumann et al. 1984; Habing et al. 2001; Zuckerman & Song 2004).”
Debris Disks around Sun-like Stars (2007, methodology): “It is well known that excess rates decrease with stellar age (Habing et al. 2001; Spangler et al. 2001; Rieke et al. 2005; Su et al. 2006; Siegler et al. 2007).”
Nearby Debris Disk Systems with High Fractional Luminosity Reconsidered (2006, background): “We note that most selected candidates have already been published by the original observers (Decin et al. 2000; Habing et al. 2001; Spangler et al. 2001; Silverstone 2000), but due to their different processing schemes, the published flux densities cannot be directly merged for a homogeneous…”
NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, unknown): “…et al. 2006; Liu et al. 2004; Weinberger et al. 2004; Song et al. 2002), the Infrared Space Observatory (ISO; de Muizon 2005; Laureijs et al. 2002; Habing et al. 2001; Spangler et al. 2001) and the Spitzer Space Telescope (Werner et al. 2004) have discovered >100 nearby stars with infrared excess.”
FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS (2008, background): “Subsequent observations with ISO demonstrated that the frequency of debris disks declines with age (Habing et al. 1999, 2001; Spangler et al. 2001).”
Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “In these disks, the small scale height of the dust,H /a 0:1, is consistent withmaterial in roughly circular orbits (e.g., Backman&Paresce1993;Kalas et al. 2004 and references therein).”
Young Stars Near the Sun (2004, background): “Young stars are more likely than older stars to be far-IR excess sources (Habing et al. 2001, Spangler et al. 2001).”
Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs (2006, methodology): “By contrast, three teams (Habing et al. 2001; Spangler et al. 2001; Decin et al. 2003) investigated the temporal evolution of the dust using the ISO database.”
Debris disks as signposts of terrestrial planet formation (2011, result): “These values are 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…”
Frequency of Debris Disks around Solar-Type Stars: First Results from a Spitzer MIPS Survey (2005, background): “Two of these three detections were previously identified by IRAS.1 Based on a more general ISO survey and IRAS data, Habing et al. (2001) compiled a larger sample for determining the fraction of solar-type stars with IR excess.”