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19 Apr 2006: 4.2. Modelingg the SED. The spectral energy distribution (SED) of Corvi from op-tical to submillimeter wavelengths is plotted in Figure 4.

21 Jan 2014: However, this similarityrequires that both components are radially optically thickand op-tically thin in the viewing direction, or the opening anglesmust belarger. ... The length of this period is uncertain due to the possibilityof non-axisymmetry and an

17 Oct 2023: ARI's TAP access to the Gaia Archive. Unique source identifier (unique within a particular Data Release) Basis function coefficients for the BP spectrum representation Basis function coefficients for the RP spectrum representation

21 Feb 2019: Gas mass calculations based on opticallythick 12CO emission can lead to underestimations of as largeas two orders of magnitude in comparison to those using op-tically thin CO isotopologues (Moór et

15 Jan 2015: arX. iv:1. 412. 0675. v1 [. astr. o-ph. EP. ] 1. Dec. 201. 4DRAF T VERS IONDECEMBER 3, 2014Preprint typeset using LATEX style emulateapj v. 5/2/11. EXO-ZODI MODELLING FOR THE LARGE BINOCULAR TELESCOPE INTERFEROMETER. GRANT M. K ENNEDY1, M ARK C.

9 Feb 2015: Golimowski D. A., Burrows C. J., Kulkarni S. R., Op-penheimer B.

19 Apr 2006: " $#%&%&' ()" #$%%'-,.0/(12&34657798:";" =<>? @$$A$>;"? BC? ";D= ;" EF46 "9/ GHJI"K"KMLBNPOQ R9SOETUQ VFW"OXTMY!Z[QS W"OXW"]BV. GTMY_OXVFW"O. (a Nb?K"K&c K"K"K"KdUe(K"K"K"K"K"K"K"K"K"K"K"K"K"K"KMe. fhgji kmlon_pqnsr turwv xzy|{|}ns{|r {|wi}_. 6sJ

12 Nov 2013: The work of OP, MCW and GMK is supported by the EuropeanUnion through ERC grant number 279973.

31 Mar 2023: MNRAS 000, 1–11 (2023) Preprint 31March 2023 Compiled usingMNRASLATEXstyle file v3.0. Stirred but not shaken: a multi-wavelength view of HD 16743’s debris disc. JonathanP.Marshall,1,2 J.Milli,3 E.Choquet,4 C. delBurgo,5 G.M.Kennedy,6,7 F.Kemper,8

23 Nov 2021: The HD J = 2 1 line is stronger for low mass op-tically thin disks (1019 W m2) and fainter for opticallythick massive disks (1018 W m2).Since the line fluxes ... Due to the lower op-tical depth with respect to the main isotopologue, the13CO transitions

27 Jul 2010: The outcome is summarisedin Fig. 6. 4.4.1 Radiation pressure. Radiation pressure is a radial force which acts in the op-posite direction to the star’s gravity.

8 Jul 2020: Finally, the detection of this gas is also a new op-portunity to study mechanisms that can transport angularmomentum in discs and may be beneficial for our under-standing of the ... We also compute CN masses in non-LTE assuming op-tically thin emission

17 Jan 2020: Evidence of misaligned inner discs has also beenrecently inferred for several systems using high-contrast op-tical/infrared images, which have revealed shadows in theouter disc cast by unseen inclined inner

23 Sep 2016: before through modelling observations of op-tical and near-IR scattered light from the dust disk (e.g.Ahmic et al.

14 Sep 2015: map reproduces the input op-tical depths very closely.

3 Nov 2008: arX. iv:0. 810. 5087. v1 [. astr. o-ph. ] 28. Oct. 200. 8Astronomy & Astrophysicsmanuscript no. 10706 c ESO 2008October 28, 2008. Resolved debris disk emission around η Tel: a young Solar Systemor ongoing planet formation? R. Smith1, L.J. Churcher1,

23 Aug 2018: 2017, Fig. A1, bottom). The high op-tical depth in the mid-plane would in fact shield the smallgrains from sublimation.

8 Nov 2011: It is interesting to note that the op-timum position for the inner planet is not as close to thestar as the outer planet could possibly scatter particles

19 Apr 2006: To probe the nature of the Vega disk further, wehave fitted it with models including realistic grain op-tical properties.

2 Nov 2015: Road, Cambridge, UK9 Department of Astronomy, Yale University, New Haven, CT10 Visiting Astronomer, NASA Infrared Telescope Facility, op-.