C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET02:50:59

2003A&A...397..595D - Astronomy and Astrophysics, volume 397, 595-609 (2003/1-2)

The dust disk of HR 4049. Another brick in the wall.


Abstract (from CDS):

We present the Spectral Energy Distribution of HR 4049 based on literature data and new continuum measurements at 850µm. The SED shows variable absorption in the UV, and a large IR excess, both caused by circumstellar dust. The shape of the IR excess from 1µm all the way down to 850µm can be nearly perfectly fitted with a single blackbody function at T≃1150K or alternatively with a sum of blackbodies in a narrow temperature range. The energy emitted in this IR continuum radiation is about one-third of the stellar luminosity. We show that this blackbody radiation must be due to the presence of a circumbinary disk with a large height. This disk must also be gas-rich, in agreement with the observations of molecular bands in the ISO-SWS spectrum. We present two possible scenario's for explaining the shape and the intensity of the IR excess. The first scenario involves large grains (a≥1mm) that each radiate like a blackbody. The second scenario argues that the blackbody radiation is due to a very optically thick circumbinary disk. We investigate if such a disk would indeed produce blackbody radiation by presenting results from radiative transfer calculations. We further quantify the properties of such a disk and its stability in the framework of (hydro)dynamics, grain settling, radiation pressure and grain drift. The virtues and shortcomings of both models for the origin of the IR blackbody are discussed by contrasting them with other observations and assessing them in the framework of (binary) (post-)AGB evolution.

Abstract Copyright:

Journal keyword(s): circumstellar matter - infrared: stars - binaries: spectroscopic - stars: evolution - stars: variables: general

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 725 0
2 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 289 0
3 HD 98800 RS* 11 22 05.28975 -24 46 39.7571   10.20 9.28 9.26 7.386 K5V(e) 335 0
4 V* HM Aqr pA* 22 35 27.5256072315 -17 15 26.885199823 9.31 9.08 8.90     A0III 102 0

    Equat.    Gal    SGal    Ecl

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