Debris Disks around Sun-like Stars

By D. Trilling, G. Bryden, C. Beichman, G. Rieke, K. Su, J. Stansberry, M. Blaylock, K. Stapelfeldt, J. Beeman, E. E. Haller. 2007

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We have observed nearly 200 FGK stars at 24 and 70 μm with the Spitzer Space Telescope. We identify excess infrared emission, including a number of cases where the observed flux is more than 10 times brighter than the predicted photospheric flux, and interpret these signatures as evidence of debris disks in those systems. We combine this sample of FGK stars with similar published results to produce a sample of more than 350 main sequence AFGKM stars. The incidence of debris disks is 4.2+ 2.0−1.1% at 24 μm for a sample of 213 Sun-like (FG) stars and 16.4+ 2.8−2.9% at 70 μm for 225 Sun-like (FG) stars. We find that the excess rates for A, F, G, and K stars are statistically indistinguishable, but with a suggestion of decreasing excess rate toward the later spectral types; this may be an age effect. The lack of strong trend among FGK stars of comparable ages is surprising, given the factor of 50 change in stellar luminosity across this spectral range. We also find that the incidence of debris disks declines very slowly beyond ages of 1 billion years.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5ead094aea94e4d659012a0679af6b0a15d01b07

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Citations in the corpus

PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, background): “…a function of stellar type (a surrogate for stellar mass) in some clusters (Lada et al. 2006; Luhman et al. 2008; S. Strom 2007, private communication), as well as an increased incidence of debris disks with increasing stellar mass (Trilling et al. 2008; Hillenbrand et al. 2008; Cieza et al. 2008).”
NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, unknown): “Carpenter et al. (2009) and Trilling et al. (2008) both note that the 70 µm age evolution for the disk frequency and – 16 – disk brightness for solar-type stars does not decrease with age as strongly as is observed for A-type stars (Su et al. 2006; Rieke et al. 2005).”
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.”
RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS (2009, background): “…stars resemble the occurrence rates of debris disks found through excess infrared emission (∼15% for Sun-like stars: Bryden et al. 2006; Trilling et al. 2008; &30% for IM stars: Rieke et al. 2005; Su et al. 2006; Morales et al. 2009), although at the moment no correlation has been…”
Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “…Bryden et al. 2006; Gorlova et al. 2006, 2007; Currie et al. 2007a; Siegler et al. 2007; Trilling et al. 2007), the frequency of excess emission declines from 30%Y40% for A-type stars (Su et al. 2006) to 10%Y20% for solar-type stars (Greaves&Wyatt 2003; Trilling et al. 2008; Meyer et al. 2008).”
Debris disc stirring by secular perturbations from giant planets (2009, methodology): “We take 57 planet-hosting stars with publishedSpitzer/MIPS photometry (Beichman et al. 2006; Moro-Martı́n et al. 2007; Trilling et al. 2008; Backman et al. 2009).”
COMETARY ORIGIN OF THE ZODIACAL CLOUD AND CARBONACEOUS MICROMETEORITES. IMPLICATIONS FOR HOT DEBRIS DISKS (2009, background): “These results have interesting implications for our understanding of hot debris disks observed within 10 AU around mature stars (Trilling et al. 2008; Meyer et al. 2008; Carpenter et al. 2009; see also a review by Wyatt 2008).”
THE TUCANA/HOROLOGIUM, COLUMBA, AB DORADUS, AND ARGUS ASSOCIATIONS: NEW MEMBERS AND DUSTY DEBRIS DISKS (2011, methodology): “To check whether our atmospheric model well reproduces actual stellar photospheres, in Figure 8 we compare the model predictions with MIPS measurements at 24 µm of a sample of nearby F, G, and K-type stars from a paper by Trilling et al. (2008).”
FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS (2008, background): “For stars older than 600 Myr, the presence of 70µm excess shows no clear dependence on spectral type for AFGK stars (Trilling et al. 2008).”
Debris disks as signposts of terrestrial planet formation (2011, background): “…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 very few systems…”
DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE STAR GJ 504 (2013, methodology): “A recent Spitzer survey showed that 4% of Sun-like stars have 24 µm excess, while 16% of Sun-like stars have 70 µm excess (Trilling et al. 2008).”
Imaging Extrasolar Giant Planets (2016, background): “Given the high incidence of debris disks around main-sequence stars (&16–20%: Trilling et al. 2008; Eiroa et al. 2013), with even higher rates at younger ages (Rieke et al. 2005; Meyer et al. 2008), any correlation of imaged giant planets and debris disks will be difficult to discern because the…”