Decay of Planetary Debris Disks

By G. Rieke, K. Su, J. Stansberry, D. Trilling, G. Bryden, J. Muzerolle, B. White, N. Gorlova, E. Young, C. Beichman and 2 more. 2005

298 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fcb1186fa9ec4090da8f5d7ce91d42433319b827

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. K. Luhman
2. Eric Mamajek
3. L. Hillenbrand
4. B. Bowler
5. L. Hartmann
6. Michael C. Liu
7. N. Calvet
8. S. Andrews

Citations in the corpus

• The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, background): “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.”
• Evidence for Mass-dependent Circumstellar Disk Evolution in the 5 Myr Old Upper Scorpius OB Association (2006, background): “MIPS 24µm surveys have detected dust in 7–48% of 10–30Myr stars (Young et al. 2004; Rieke et al. 2005; Chen et al. 2005), but with fractional dust luminosities orders of magnitude below that found in younger sources.”
• FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS (2008, background): “Rieke et al. (2005) found that ∼ 47% of A-type stars younger than 90 Myr have a 24µm excess more than 25% above the photosphere, with a rapid decline in both the frequency and magnitude of the excess toward older ages.”
• A Spitzer Space Telescope Study of Disks in the Young σ Orionis Cluster (2007, methodology): “Finally, the intermediateexcess region 0:5 < K 24½ < 3:3 is consistent with colors typical of optically thin debris disks (the famous Pic debris disk system, which is one of the debris disk systems with the largest 24 m excess known, has K 24½ 3:3; e.g., Gorlova et al. 2004; Rieke et al. 2005).”
• Astrobiology: The Study of the Living Universe (2005, background): “[There is now observational evidence that large planetesimal collisions in other solar systems are common at the end of planetary accretion (Rieke et al. 2005), but, of course, there are currently no statistical data about the frequency or nature of planet–moon combinations that may result.]”
• Transience of Hot Dust around Sun-like Stars (2006, methodology): “…off ∝ t−1.8 (Spangler et al. 2001); the mass inferred from detection statistics falls off ∝ t−0.5 (Greaves & Wyatt 2003), while the mass of the detected disks falls off ∝ t−1 (Najita & Williams 2005); the upper limit in luminosity of the detected disks also falls off ∝ t−1 (Rieke et al. 2005).”
• A Spitzer View of Protoplanetary Disks in the γ Velorum Cluster (2008, methodology): “We use the color K[24] to determine the excess ratio at 24µm (e.g., Rieke et al. 2005), E24 = 10 (K−[24]−0.05)/2.5, where 0.05 is the mean value of K-[24] for the photometric candidates with MIPS detections.”
• Debris Disks in Main-Sequence Binary Systems (2006, methodology): “There are extensive programs with the Spitzer Space Telescope to study debris disks around single stars (e.g., Beichman et al. 2005a, 2005b; Rieke et al. 2005; Kim et al. 2005; Bryden et al. 2006; Su et al. 2006), but binaries—a majority of solar-type stars—have generally been explicitly omitted…”
• Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, background): “Our study differs – 20 – from these in the Rieke et al. (2005) and the Najita & Williams (2005) samples in that (1) our sample contains a heterogenous mix of stars with varying spectral type and (2) our data set includes the measurement of the excess at more than one wavelength; the measurement of…”
• Irregular Satellites of the Planets: Products of Capture in the Early Solar System (2007, background): “Erratic dust production, possibly owing to collisions between large bodies, decays on timescales ten times longer (see Rieke et al. 2005).”
• Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs (2006, unknown): “The Rieke et al. (2005) Spitzer survey at 24 m included three Algols.”
• Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, background): “However, recent discoveries as diverse as icy ∼Neptune-mass planets orbiting M dwarfs (e.g. Rivera et al. 2005), and debris disks around A-type stars (e.g. Rieke et al. 2005) show that planet formation occurs over a wide range of spectral types.”
• Nearby Debris Disk Systems with High Fractional Luminosity Reconsidered (2006, methodology): “Recently Rieke et al. (2005) presented a survey of A-type stars, performed at 24 m with the Multiband Imaging Photometer for Spitzer (MIPS; Rieke et al. 2004) on board the Spitzer Space Telescope (Werner et al. 2004), and observed a general decay on a timescale of 150 Myr.”
• The Complete Census of 70 μm-Bright Debris Disks within “The Formation and Evolution of Planetary Systems” Spitzer Legacy Survey of Sun-like Stars (2007, result): “These findings are consistent with the relative detection frequencies of debris among A star samples, FGK samples, and M star samples having a wide range of ages (e.g., Rieke et al. 2005; Meyer et al. 2008; Gautier et al. 2007).”
• Absolute Calibration and Characterization of the Multiband Imaging Photometer for Spitzer. I. The Stellar Calibrator Sample and the 24 μm Calibration (2007, methodology): “For example, the MIPS 24 µm channel allows measurement of infrared excesses around stars with lower effective temperatures and/or lower-mass debris disks than previously possible (e.g., Rieke et al. 2005; Bryden et al. 2006).”