Many stars are surrounded by gaseous and dusty disk. The gaseous disk regions
often display forbidden emission lines and produce measurable amounts of
molecular emission, e.g., in CO. The dust parts cause
on the one hand strong continuum emission noticeable via an infrared excess,
but also spectral features corresponding to vibrational transitions
in small dust particles.
Our investigations aim at finding tracers for all disk regions. Hence, we
study the circumstellar disks over the complete wavelength range, extending
from the optical to the infrared. The optical range hosts several forbidden
emission lines that were identified as valuable tracers for the innermost
disk regions, i.e., close to the star.
For the molecular disk regions, we studied so far the CO band emission in great
detail, in order to constrain the disk parameters such as density and temperature,
but also to derive proper kinematical information (Keplerian rotation versus
outflow).
We study the disks of evolved massive stars using both observations in different
wavelength regions, but we also developed our theoretical models and numerical
codes. Below is a selection of our results on
Ionized and neutral atomic disk region
We found that several sets of optical forbidden emission lines can be used
as valuable tracers for the structure and the kinematics of the innermost
disk regions. These are the lines of [OI] and [CaII].
[OI] - Kraus, Borges Fernandes & de Araújo, 2007, A&A 463, 627
& Kraus, Borges Fernandes & de Araújo, 2010, A&A 517, A30
[CaII] - Aret, Kraus, Muratore, Borges Fernandes, 2012, MNRAS, 423, 284
Molecular disk region
A description of the code developed to model CO band emission from disks and
winds is described in the following publication:
CO band emission from MWC 349 - Kraus, Krügel, Thum, & Geballe, 2000, A&A, 362, 158
Applications to the molecular disks of evolved massive stars can be found in a
variety of publications, e.g.,
CPD-52 9243 - Cidale, Borges Fernandes, Andruchow, Arias, Kraus, Chesneau, Kanaan, Curé, de Wit, & Muratore, 2012, A&A, 548, A72
GG Car - Kraus, Oksala, Nickeler, Muratore, Borges Fernandes, Aret, Cidale,
de Wit, 2013, A&A, 549, A28
The CO bands are also found to be ideal age indicators
The 13Carbon footprint of B[e] supergiants - Kraus, 2009, A&A, 494, 253 & Liermann, Kraus, Schnurr, & Borges Fernandes, 2010, MNRAS, 408, L6
Dusty disks
Detailed descriptions of the radiative transfer codes developed and used to study
the structure of the dusty disks is described in the following two publications:
SEDs of flared dust disks - Kraus, 2003, in Open Issues in Local Star Formation, p. 279
The dusty disk of CD-42 11721 - Borges Fernandes, Kraus, Lorenz Martins, & de Araújo, 2007, MNRAS, 377, 1343