Erratum: “SpitzerIRS Spectroscopy ofIRAS‐Discovered Debris Disks” (ApJS, 166, 351, [2006])

Abstract

We also mis-reported the temperature of the silicate and carbon grains in our fit to the HR 7012 IRS spectrum; the grains have a temperature 550 K, not 520 K as reported previously. Lastly, the composition of the enstatite used to fit the HR 7012 spectrum is Mg 0.7 Fe 0.3 SiO 3 , not Mg 0.7 Fe 0.3 SiO 4 . In addition, we noticed an error in the minimum blow-out size for silicate, carbon, and silica grains around HD 113766 and HR 7012; the blow-out sizes are smaller than previously estimated. For HD 113766, we originally estimated minimum silicate and carbon sizes of 1.4 and 1.9 m, respectively; we now estimate 0.35 and 0.46 m, respectively. With the exception of forsterite, all of the grains used to model the HD 113766 spectrum are larger than the minimum grain sizes. The forsterite grains (submicron) possess radii that are similar to the minimum silicate grain size. For HR 7012, we originally estimated minimum silicate, carbon, and silica sizes of 1.1, 1.4, and 1.6 m, respectively; we now estimate 0.9, 1.2, and 1.3 m, respectively. The enstatite and cristobalite grains used to model the infrared HR 7012 spectrum are still smaller than the minimum grain size. We had previously concluded that the minimum grain sizes (>1 m) were inconsistent with presence of submicron-sized grains inferred from the structure of the silicate emission features, suggesting that a recent massive collision must have occurred around HD 113766 and HR 7012. Our new minimum grain size estimates are more consistent with our models for the infrared spectra and do not require a recent massive collision around HD 113766. However, our models do indicate the presence of submicron-sized particles significantly smaller than the blow-out size around HR 7012, suggesting that a recent massive collision may have occurred in this system.

Kuiper belts around nearby stars

“…The 800 μm flux measured for HD 141569 (red marker) at CSO (Walker & Butner 1995) has been left out of the fit since it is probably incorrect. References: HD 105 (Moór et al 2006;Hillenbrand et al 2008;Carpenter et al 2005;Cutri et al 2003); HD 21997 (Moór et al 2006;Williams & Andrews 2006;Cutri et al 2003); HD 30447 (Moór et al 2006;Cutri et al 2003); HD 95086 (Chen et al 2006;Cutri et al 2003); HD 98800 (Low et al 2005;Schütz et al 2005;Mannings & Barlow 1998;Cutri et al 2003;Walker & Heinrichsen 2000;Gregorio-Hetem et al 1992;Garcia-Lario et al 1990;Sylvester et al 1996;Cieza 2008;Sylvester et al 2001); HD 109573 (Moór et al 2006;Sheret et al 2004;Barrado Y Navascués 2006;Cutri et al 2003;Low et al 2005;Jura et al 1995;Telesco et al 2000;Jura et al 1993;Fajardo-Acosta et al 1998;Wahhaj et al 2005); HD 131835 (Moór et al 2006;Cutri et al 2003); HD 141569 (Sylvester et al 2001(Sylvester et al , 1996Beichman et al 1988;Walker & Butner 1995;Sheret et al 2004); HD 152404 (Chen et al 2005;…”

Chemical depletion in the Large Magellanic Cloud: RV Tauri stars and the photospheric feedback from their dusty discs

“…Debris discs have been found around main-sequence stars of all spectral types (e.g. Bryden et al 2006;Chen et al 2006).…”

Gas and dust in the beta Pictoris moving group as seen by theHerschelSpace Observatory

“…Although dust has been extensively observed, studies have provided little information about its chemical composition. So far, only a few debris discs have shown solid-state features in their mid-IR spectra, indicating the presence of small and warm grains (Chen et al 2006;Fujiwara et al 2013). These debris discs are most probably in a transient state, and the small dust grains are produced during periods of intense collisional grinding (Lisse et al 2008(Lisse et al , 2009.…”