Scattering by Interstellar Dust Grains. I. Optical and Ultraviolet

By B. Draine. 2003

485 citations recorded by the source corpus.

Scattering and absorption properties at optical and ultraviolet wavelengths are calculated for an interstellar dust model consisting of carbonaceous grains and amorphous silicate grains. Polarization as a function of scattering angle is calculated for selected wavelengths from the infrared to the vacuum ultraviolet. The widely used Henyey-Greenstein phase function provides a good approximation for the scattering phase function at wavelengths between ~0.4 and 1 μm but fails to fit the calculated phase functions at shorter and longer wavelengths. A new analytic phase function is presented. It is exact at long wavelengths and provides a good fit to the numerically calculated phase function for λ > 0.27 μm. Observational determinations of the scattering albedo and ⟨cos θ⟩ show considerable disagreement, especially in the ultraviolet. Possible reasons for this are discussed.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/e5baf56960edd21e28910262c8332c84f19f32d9

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

In Atmospheric Science

Citations in the corpus

Lyman α radiative transfer in a multiphase medium (2005, methodology): “Let n̂ be the direction of 3 Draine (2003) shows that the Henyey–Greenstain distribution is inaccurate for wavelengths λ 4700 Å.”
Photodissociation and photoionisation of atoms and molecules of astrophysical interest (2017, methodology): “These were taken from the mixed grain-size and composition model developed by Draine et al. (Draine & Lee 1984; Li & Draine 2001; Weingartner & Draine 2001; Draine 2003a,b,c).”
Three-Dimensional Dust Radiative Transfer ∗ (2013, background): “This review discusses the physical properties of dust only in the context of RT and the modeling of objects; for other aspects mentioned above, we refer the reader to any one of the many published works on dust (e.g. Draine 2003a; Henning 2010; Henning, Grün & Steinacker 2009).”
Kinematic Evidence for an Embedded Protoplanet in a Circumstellar Disk (2018, methodology): “We assumed a population of astrosilicate (Draine 2003) grains with sizes ranging from 0.03 to 1000µm and following a power-law dn(a) ∝ a−3.5da, a gas-to-dust ratio of 100, and computed the dust optical properties using Mie theory.”
AGN Dusty Tori. I. Handling of Clumpy Media (2008, methodology): “The optical constants for graphite are from Draine (2003), for silicate from the Ossenkopf, Henning, & Mathis (1992) “cold dust”, which produces better agreement with observations of the 10 and 18µm silicate features (Sirocky et al. 2008).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “…Madden et al., 2006); (ii) the variations in the RV parameter of the extinction curve is interpreted as variations of the grain size distribution (Draine, 2003a; Fitzpatrick & Massa, 2005); (iii) coagulation occurs in dense regions (e.g. Stepnik et al., 2003; Berné et al., 2007); (iv) blast…”
A UNIFIED REPRESENTATION OF GAS-PHASE ELEMENT DEPLETIONS IN THE INTERSTELLAR MEDIUM (2009, background): “About twice this amount is needed to explain the dust extinction (Draine 2003a).”
Cold Disks: Spitzer Spectroscopy of Disks around Young Stars with Large Gaps (2007, methodology): “Optical andRgap, out (sub)millimeter photometry is often not simultaneous and is dereddened using the extinction law of Draine (2003).”
Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? - SAO 206462 (HD 135344B) in polarized light with VLT/NACO (2013, background): “Since the degree of linear polarization is maximized at∼ 90◦ scattering angle (e.g. Draine 2003; Min et al. 2012), polarized images of inclined disks are indeed expected to show minima along the near and far side of the disk (see case of MWC480, Kusakabe et al. 2012).”
Low RV from Circumstellar Dust around Supernovae (2008, methodology): “For quasar sight-lines, Östman et al. (2008) tested both Milky-Way like extinction as well as Small Magellanic Cloud (SMC) extinction law, both giving comparable goodness of fit.”
Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “The mass extinction coefficients are calculated using Mie theory with the miex code (Wolf & Voshchinnikov 2004) and optical constants by Draine (2003) for graphite and Weingartner & Draine (2001) for silicates.”
FEEDBACK IN LUMINOUS OBSCURED QUASARS (2011, methodology): “…measurement is sensitive to the assumed gas-to-dust ratio and the scattering angle (for this particular value, 90◦ and Small Magellanic Cloud dust, Draine 2003), but nevertheless it is clear that the scattered light observations require muchlower densities than those implied by [SII ] ratios.”
POLARIZED FAR-INFRARED AND SUBMILLIMETER EMISSION FROM INTERSTELLAR DUST (2008, background): “Our knowledge of interstellar dust has advanced considerably since then, but remains incomplete [see, e.g., the review by Draine (2003), or the book by Whittet (2003)].”
Smooth and clumpy dust distributions in AGN: a direct comparison of two commonly explored infrared emission models (2012, background): “…(see e.g. Mor et al. 2009; Nikutta et al. 2009; Deo et al. 2011; Ramos-Almeida et al. 2011; Esquej et al. 2012), assume a grain composition of 53% silicate and 47% graphite, with the optical constants for the graphite taken from Draine (2003) and that of the silicates from Ossenkopf et al. (1992).”
Scattering by Interstellar Dust Grains. II. X-Rays (2003, background): “The nature of interstellar grains remains uncertain (see Draine 2003a, and references therein).”