2001A&A...375..455L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST00:28:10

2001A&A...375..455L - Astronomy and Astrophysics, volume 375, 455-468 (2001/8-4)

The spectral energy distribution of self-gravitating protostellar disks.

LODATO G. and BERTIN G.

Abstract (from CDS):

The long wavelength emission of protostellar objects is commonly attributed to a disk of gas and dust around the central protostar. In the first stages of disk accretion or in the case of high mass protostars, the disk mass is likely to be sufficiently large, so that the disk self-gravity may have an impact on the dynamics and the emission properties of the disk. In this paper we describe the spectral energy distribution (SED) produced by a simple, non-flaring, self-gravitating accretion disk model. Self-gravity is included in the calculation of the rotation curve of the disk and in the energy balance equation, as a term of effective heating related to Jeans instability. In order to quantify in detail the requirements on the mass of the disk and on the accretion rate posed on the models by realistic situations, we compare the SEDs produced by these models with the observed SEDs of a small sample of well-studied protostellar objects. We find that relatively modest disks - even lighter than the central star - can lead to an interesting fit to the infrared SED of the FU Orionis objects considered, while in the case of T Tauri stars the required parameters fall outside the range suggested as acceptable by the general theoretical and observational scenario. On the basis of the present results, we may conclude that the contribution of a self-gravitating disk is plausible in several cases (in particular, for FU Orionis objects) and that, in the standard irradiation, dominated disk scenario, it would help soften the requirements encountered by Keplerian accretion models.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - gravitation - stars: pre-main sequence

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 599 0
2 V* DE Tau Or* 04 21 55.6346296353 +27 55 06.184221341 15.18 15.13 13.80     M3Ve 222 0
3 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1249 2
4 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
5 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
6 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1201 0
7 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
8 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 467 0
9 V* FU Ori Or* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 708 1
10 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
11 V* V1515 Cyg Or* 20 23 48.0159810586 +42 12 25.780858811   15.26 13.39 12.03   G0/G2Ib 211 0
12 EM* LkHA 190 Or* 20 58 53.7336698326 +44 15 28.384667940   14.26 12.33 12.13   F7/G3I/IIe 476 0
13 V* V1735 Cyg Or* 21 47 20.6624829527 +47 32 03.856911703           ~ 152 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-00:28:10

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