Strong irradiation of protostellar cores in Corona Australis

Johan Lindberg; Jes Kristian Jørgensen

doi:10.1051/0004-6361/201219603

Strong irradiation of protostellar cores in Corona Australis

Johan Lindberg, Jes Kristian Jørgensen

Astrofysik og Planetforskning

22 Citationer (Scopus)

55 Downloads (Pure)

Abstract

Context. The importance of the physical environment in the evolution of newly formed low-mass stars remains an open question. In particular, radiation from nearby more massive stars may affect both the physical and chemical structure of these kinds of young stars. Aims. We constrain the physical characteristics of a group of embedded low-mass protostars in Corona Australis in the vicinity of the young luminous Herbig Be star R CrA. Methods. Millimetre wavelength maps of molecular line and continuum emission towards the low-mass star forming region IRS7 near R CrA from the Submillimeter Array (SMA) and Atacama Pathfinder Experiment (APEX) are presented. The maps show the distribution of 18 lines from 7 species (H₂CO, CH₃OH, HC₃N, c-C₃H₂, HCN, CN and SiO) on scales from 3′′ to 60′′ (400-8000 AU). Using a set of H ₂CO lines, we estimate the temperatures and column densities in the region using both LTE and non-LTE methods. The results are compared with 1-D radiative transfer modelling of the protostellar cores. These models constrain which properties of the central source, protostellar envelope, and surrounding radiation field can give rise to the observed line and continuum emission. Results. Most of the H₂CO emission from the regions emerges from two elongated (~6000 AU long) narrow (<1500 AU) ridges dominating the emission picked up in both interferometric and single-dish measurements. The temperatures inferred from the H₂CO lines are no less than ∼30 K and more likely 50-60 K, and the line emission peaks are offset by ∼2500 AU from the location of the embedded protostars. These temperatures can not be explained by the heating from the young stellar objects (YSOs) themselves. Irradiation by the nearby Herbig Be star R CrA could, however, explain these high temperatures. The elevated temperatures can in turn impact the physical and chemical characteristics of protostars, in particular, lead to enhanced abundances of typical tracers of photon dominated regions (PDRs) such as seen in single-dish line surveys of embedded protostars in the region.

Originalsprog	Engelsk
Artikelnummer	A24
Tidsskrift	Astronomy & Astrophysics
Vol/bind	548
Antal sider	21
ISSN	0004-6361
DOI	https://doi.org/10.1051/0004-6361/201219603
Status	Udgivet - 1 dec. 2012

Adgang til dokumentet

10.1051/0004-6361/201219603Licens: Andet

Lindberg_2012_Strong_irradiationForlagets udgivne version, 1,99 MBLicens: Andet

Citationsformater

@article{26a1504efc1146639e330ac58353f2e5,

title = "Strong irradiation of protostellar cores in Corona Australis",

abstract = "Context. The importance of the physical environment in the evolution of newly formed low-mass stars remains an open question. In particular, radiation from nearby more massive stars may affect both the physical and chemical structure of these kinds of young stars. Aims. We constrain the physical characteristics of a group of embedded low-mass protostars in Corona Australis in the vicinity of the young luminous Herbig Be star R CrA. Methods. Millimetre wavelength maps of molecular line and continuum emission towards the low-mass star forming region IRS7 near R CrA from the Submillimeter Array (SMA) and Atacama Pathfinder Experiment (APEX) are presented. The maps show the distribution of 18 lines from 7 species (H2CO, CH3OH, HC3N, c-C3H2, HCN, CN and SiO) on scales from 3′′ to 60′′ (400-8000 AU). Using a set of H 2CO lines, we estimate the temperatures and column densities in the region using both LTE and non-LTE methods. The results are compared with 1-D radiative transfer modelling of the protostellar cores. These models constrain which properties of the central source, protostellar envelope, and surrounding radiation field can give rise to the observed line and continuum emission. Results. Most of the H2CO emission from the regions emerges from two elongated (~6000 AU long) narrow (<1500 AU) ridges dominating the emission picked up in both interferometric and single-dish measurements. The temperatures inferred from the H2CO lines are no less than ∼30 K and more likely 50-60 K, and the line emission peaks are offset by ∼2500 AU from the location of the embedded protostars. These temperatures can not be explained by the heating from the young stellar objects (YSOs) themselves. Irradiation by the nearby Herbig Be star R CrA could, however, explain these high temperatures. The elevated temperatures can in turn impact the physical and chemical characteristics of protostars, in particular, lead to enhanced abundances of typical tracers of photon dominated regions (PDRs) such as seen in single-dish line surveys of embedded protostars in the region.",

author = "Johan Lindberg and J{\o}rgensen, {Jes Kristian}",

year = "2012",

month = dec,

day = "1",

doi = "10.1051/0004-6361/201219603",

language = "English",

volume = "548",

journal = "Astronomy and Astrophysics Supplement Series",

issn = "0004-6361",

publisher = "E D P Sciences",

}

TY - JOUR

T1 - Strong irradiation of protostellar cores in Corona Australis

AU - Lindberg, Johan

AU - Jørgensen, Jes Kristian

PY - 2012/12/1

Y1 - 2012/12/1

N2 - Context. The importance of the physical environment in the evolution of newly formed low-mass stars remains an open question. In particular, radiation from nearby more massive stars may affect both the physical and chemical structure of these kinds of young stars. Aims. We constrain the physical characteristics of a group of embedded low-mass protostars in Corona Australis in the vicinity of the young luminous Herbig Be star R CrA. Methods. Millimetre wavelength maps of molecular line and continuum emission towards the low-mass star forming region IRS7 near R CrA from the Submillimeter Array (SMA) and Atacama Pathfinder Experiment (APEX) are presented. The maps show the distribution of 18 lines from 7 species (H2CO, CH3OH, HC3N, c-C3H2, HCN, CN and SiO) on scales from 3′′ to 60′′ (400-8000 AU). Using a set of H 2CO lines, we estimate the temperatures and column densities in the region using both LTE and non-LTE methods. The results are compared with 1-D radiative transfer modelling of the protostellar cores. These models constrain which properties of the central source, protostellar envelope, and surrounding radiation field can give rise to the observed line and continuum emission. Results. Most of the H2CO emission from the regions emerges from two elongated (~6000 AU long) narrow (<1500 AU) ridges dominating the emission picked up in both interferometric and single-dish measurements. The temperatures inferred from the H2CO lines are no less than ∼30 K and more likely 50-60 K, and the line emission peaks are offset by ∼2500 AU from the location of the embedded protostars. These temperatures can not be explained by the heating from the young stellar objects (YSOs) themselves. Irradiation by the nearby Herbig Be star R CrA could, however, explain these high temperatures. The elevated temperatures can in turn impact the physical and chemical characteristics of protostars, in particular, lead to enhanced abundances of typical tracers of photon dominated regions (PDRs) such as seen in single-dish line surveys of embedded protostars in the region.

AB - Context. The importance of the physical environment in the evolution of newly formed low-mass stars remains an open question. In particular, radiation from nearby more massive stars may affect both the physical and chemical structure of these kinds of young stars. Aims. We constrain the physical characteristics of a group of embedded low-mass protostars in Corona Australis in the vicinity of the young luminous Herbig Be star R CrA. Methods. Millimetre wavelength maps of molecular line and continuum emission towards the low-mass star forming region IRS7 near R CrA from the Submillimeter Array (SMA) and Atacama Pathfinder Experiment (APEX) are presented. The maps show the distribution of 18 lines from 7 species (H2CO, CH3OH, HC3N, c-C3H2, HCN, CN and SiO) on scales from 3′′ to 60′′ (400-8000 AU). Using a set of H 2CO lines, we estimate the temperatures and column densities in the region using both LTE and non-LTE methods. The results are compared with 1-D radiative transfer modelling of the protostellar cores. These models constrain which properties of the central source, protostellar envelope, and surrounding radiation field can give rise to the observed line and continuum emission. Results. Most of the H2CO emission from the regions emerges from two elongated (~6000 AU long) narrow (<1500 AU) ridges dominating the emission picked up in both interferometric and single-dish measurements. The temperatures inferred from the H2CO lines are no less than ∼30 K and more likely 50-60 K, and the line emission peaks are offset by ∼2500 AU from the location of the embedded protostars. These temperatures can not be explained by the heating from the young stellar objects (YSOs) themselves. Irradiation by the nearby Herbig Be star R CrA could, however, explain these high temperatures. The elevated temperatures can in turn impact the physical and chemical characteristics of protostars, in particular, lead to enhanced abundances of typical tracers of photon dominated regions (PDRs) such as seen in single-dish line surveys of embedded protostars in the region.

U2 - 10.1051/0004-6361/201219603

DO - 10.1051/0004-6361/201219603

M3 - Journal article

SN - 0004-6361

VL - 548

JO - Astronomy and Astrophysics Supplement Series

JF - Astronomy and Astrophysics Supplement Series

M1 - A24

ER -

Strong irradiation of protostellar cores in Corona Australis

Abstract

Adgang til dokumentet

Fingeraftryk

Citationsformater