J/A+A/318/879 IR photometry of L1551/IRS5 (Men'shchikov+ 1997)
Radiation transfer in circumstellar disks
Men'shchikov A.B., Henning T.
<Astron. Astrophys. 318, 879 (1997)>
=1997A&A...318..879M 1997A&A...318..879M (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Photometry, infrared
Keywords: radiative transfer - methods: numerical - circumstellar matter -
stars: individual: L1551 IRS 5
Description:
We describe a new approach to the solution of the frequency-dependent
stationary radiative transfer equation for axially-symmetric
circumstellar dust disks. The method is applied to flared disks which
are considered here as spheres with the polar cones removed. We have
simplified the problem by computing the moments of the specific
intensity only for the midplane and the surface of the flared disk. At
the same time, we solve the radiative transfer equation exactly for an
"equivalent" spherical envelope. The basic assumption is that
density distribution in the disk depends only on the radial distance
from the central star. This results in significantly faster
calculations, reduces necessary computer memory, and allows
incorporation of the algorithm into a hydrodynamical code. We applied
our fast 2D radiative transfer code to a detailed modeling of the
deeply embedded young stellar object (YSO) L1551 IRS 5. This is a YSO
in the Taurus-Aurigae star-forming region, which has been very well
studied with good spatial resolution and photometric data over the
wide range from ultraviolet to millimeter wavelengths. Exploring the
parameter space of our axially-symmetric models, we have found a
self-consistent solution for L1551 IRS 5 explaining all available
infrared and submm/mm continuum observations.
Here, Appendices A, B, and C are presented, which are not available in
the journal version of the paper. In Appendices A and B, one can find
more details on the method and the overall iterative numerical scheme.
Appendix C (Table C1) lists all published photometric observations of
L1551 IRS 5, which we have found in the literature and which have been
used in our modeling.
Objects:
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RA (2000) DE Designation(s)
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04 31 33.5 +18 08 15 LDN 1551 IRS 5 = IRAS 04287+1801
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
appena.tex 77 259 Details of the method
appenb.tex 75 248 Iterative scheme
appenc.tex 119 122 Photometry of L1551 IRS 5
tablec1 141 72 Photometry of L1551 IRS 5 (from Appendix C)
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Byte-by-byte Description of file: tablec1
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Bytes Format Units Label Explanations
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1- 8 F8.2 um lambda Wavelength of observations
10- 18 F9.4 Jy flux Observed flux
20- 29 F10.5 Jy e_flux Flux uncertainty (1)
31- 37 F7.2 arcsec AppFlux Aperture (beam size FWHM)
40- 46 A7 --- r_flux Abbreviated bibliographic reference
50-141 A92 --- Ref Full bibliographic reference
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Note (1): In few cases, when observers gave no information on accuracy
of the measurements, the flux uncertainty is set to 0.
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Acknowledgements: Alexander Men'shchikov
(End) Alexander Men'shchikov [MPG AG "Staub...", Jena] 20-May-1996