The influence of dust formation modelling on Na I and K I line profiles in substellar atmospheres

C. M. S. Johnas; Ch. Helling; M. Dehn; Peter Woitke; P. H. Hauschildt

doi:10.1111/j.1745-3933.2008.00447.x

The influence of dust formation modelling on Na I and K I line profiles in substellar atmospheres

C. M. S. Johnas, Ch. Helling, M. Dehn, Peter Woitke, P. H. Hauschildt

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

We aim to understand the correlation between cloud formation and alkali line formation in substellar atmospheres. We perform line profile calculations for Na I and KI based on the coupling of our kinetic model for the formation and composition of dust grains with 1D radiative transfer calculations in atmosphere models for brown dwarfs and giant gas planets. The Na I and KI line profiles sensibly depend on the way clouds are treated in substellar atmosphere simulations. The kinetic dust formation model results in the highest pseudo-continuum compared to the limiting cases.

Original language	English
Number of pages	5
Journal	Monthly Notices of the Royal Astronomical Society
Volume	385
DOIs	https://doi.org/10.1111/j.1745-3933.2008.00447.x
Publication status	Published - 21 Mar 2008

Keywords

line : profiles
stars : atmospheres
stars : low-mass, brown dwarfs
BROWN
HYDROGEN
GRAINS

Access to Document

10.1111/j.1745-3933.2008.00447.x

Cite this

@article{0f315be35e274dccb797cf7360ba2c9a,

title = "The influence of dust formation modelling on Na I and K I line profiles in substellar atmospheres",

abstract = "We aim to understand the correlation between cloud formation and alkali line formation in substellar atmospheres. We perform line profile calculations for Na I and KI based on the coupling of our kinetic model for the formation and composition of dust grains with 1D radiative transfer calculations in atmosphere models for brown dwarfs and giant gas planets. The Na I and KI line profiles sensibly depend on the way clouds are treated in substellar atmosphere simulations. The kinetic dust formation model results in the highest pseudo-continuum compared to the limiting cases.",

keywords = "line : profiles, stars : atmospheres, stars : low-mass, brown dwarfs, BROWN, HYDROGEN, GRAINS",

author = "Johnas, {C. M. S.} and Ch. Helling and M. Dehn and Peter Woitke and Hauschildt, {P. H.}",

year = "2008",

month = mar,

day = "21",

doi = "10.1111/j.1745-3933.2008.00447.x",

language = "English",

volume = "385",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

}

TY - JOUR

T1 - The influence of dust formation modelling on Na I and K I line profiles in substellar atmospheres

AU - Johnas, C. M. S.

AU - Helling, Ch.

AU - Dehn, M.

AU - Woitke, Peter

AU - Hauschildt, P. H.

PY - 2008/3/21

Y1 - 2008/3/21

N2 - We aim to understand the correlation between cloud formation and alkali line formation in substellar atmospheres. We perform line profile calculations for Na I and KI based on the coupling of our kinetic model for the formation and composition of dust grains with 1D radiative transfer calculations in atmosphere models for brown dwarfs and giant gas planets. The Na I and KI line profiles sensibly depend on the way clouds are treated in substellar atmosphere simulations. The kinetic dust formation model results in the highest pseudo-continuum compared to the limiting cases.

AB - We aim to understand the correlation between cloud formation and alkali line formation in substellar atmospheres. We perform line profile calculations for Na I and KI based on the coupling of our kinetic model for the formation and composition of dust grains with 1D radiative transfer calculations in atmosphere models for brown dwarfs and giant gas planets. The Na I and KI line profiles sensibly depend on the way clouds are treated in substellar atmosphere simulations. The kinetic dust formation model results in the highest pseudo-continuum compared to the limiting cases.

KW - line : profiles

KW - stars : atmospheres

KW - stars : low-mass, brown dwarfs

KW - BROWN

KW - HYDROGEN

KW - GRAINS

UR - http://www.scopus.com/inward/record.url?scp=52049097886&partnerID=8YFLogxK

U2 - 10.1111/j.1745-3933.2008.00447.x

DO - 10.1111/j.1745-3933.2008.00447.x

M3 - Article

SN - 0035-8711

VL - 385

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

ER -

The influence of dust formation modelling on Na I and K I line profiles in substellar atmospheres

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this