The outbursting protostar 2MASS 22352345 + 7517076 and its environment

M. Kun, P. Ábrahám, J. A. Acosta Pulido, A. Moór, T. Prusti

Research output: Article

1 Citation (Scopus)

Abstract

We studied the Class I protostar 2MASS 22352345 + 7517076 whose dramatic brightening between the IRAS, Akari, and WISE surveys was reported by Onozato et al. 2MASS 22352345+7517076 is a member of a small group of low-mass young stellar objects, associated with IRAS 22343 + 7501 in the molecular cloud Lynds 1251. The IRAS, ISO, Spitzer, Akari, Herschel, and WISE missions observed different stages of its outburst. Supplemented these data with archival and our own near-infrared observations, and considering the contributions of neighbouring sources to the mid-infrared fluxes we studied the nature and environment of the outbursting object, and its photometric variations from 1983 to 2017. The low-state bolometric luminosity L bol ≈32 L is indicative of a 1.6-1.8 M⊙, 1-2 × 10 5 -yr old protostar. Its 2-μm brightness started rising between 1993 and 1998, reached a peak in 2009-2011, and started declining in 2015. Changes in the spectral energy distribution suggest that the outburst was preceded by a decade-long, slow brightening in the near-infrared. The actual accretion burst occurred between 2004 and 2007. We fitted the spectral energy distribution in the bright phases with simple accretion disc models. The modelling suggested an increase of the disc accretion rate from ~3.5 × 10 -7 M ⊙ yr -1 to ~1.1 × 10 -4 M ⊙ yr -1 . The central star accreted nearly 10 -3 M ⊙, about a Jupiter mass during the 10 yr of the outburst. We observed H 2 emission lines in the K-band spectrum during the fading phase in 2017. The associated optical nebulosity RNO 144 and the Herbig-Haro object HH 149 have not exhibited significant variation in shape and brightness during the outburst.

Original languageEnglish
Pages (from-to)4424-4437
Number of pages14
JournalMonthly Notices of the Royal Astronomical Society
Volume483
Issue number4
DOIs
Publication statusPublished - márc. 11 2019

Fingerprint

protostars
Infrared Astronomy Satellite
outburst
Wide-field Infrared Survey Explorer
spectral energy distribution
accretion disks
accretion
brightness
Herbig-Haro objects
near infrared
fading
extremely high frequencies
molecular clouds
Jupiter (planet)
bursts
luminosity
Jupiter
energy
stars
modeling

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

The outbursting protostar 2MASS 22352345 + 7517076 and its environment. / Kun, M.; Ábrahám, P.; Acosta Pulido, J. A.; Moór, A.; Prusti, T.

In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 4, 11.03.2019, p. 4424-4437.

Research output: Article

@article{359644a404be46e9beb8695ad43b6cf0,
title = "The outbursting protostar 2MASS 22352345 + 7517076 and its environment",
abstract = "We studied the Class I protostar 2MASS 22352345 + 7517076 whose dramatic brightening between the IRAS, Akari, and WISE surveys was reported by Onozato et al. 2MASS 22352345+7517076 is a member of a small group of low-mass young stellar objects, associated with IRAS 22343 + 7501 in the molecular cloud Lynds 1251. The IRAS, ISO, Spitzer, Akari, Herschel, and WISE missions observed different stages of its outburst. Supplemented these data with archival and our own near-infrared observations, and considering the contributions of neighbouring sources to the mid-infrared fluxes we studied the nature and environment of the outbursting object, and its photometric variations from 1983 to 2017. The low-state bolometric luminosity L bol ≈32 L ⊙ is indicative of a 1.6-1.8 M⊙, 1-2 × 10 5 -yr old protostar. Its 2-μm brightness started rising between 1993 and 1998, reached a peak in 2009-2011, and started declining in 2015. Changes in the spectral energy distribution suggest that the outburst was preceded by a decade-long, slow brightening in the near-infrared. The actual accretion burst occurred between 2004 and 2007. We fitted the spectral energy distribution in the bright phases with simple accretion disc models. The modelling suggested an increase of the disc accretion rate from ~3.5 × 10 -7 M ⊙ yr -1 to ~1.1 × 10 -4 M ⊙ yr -1 . The central star accreted nearly 10 -3 M ⊙, about a Jupiter mass during the 10 yr of the outburst. We observed H 2 emission lines in the K-band spectrum during the fading phase in 2017. The associated optical nebulosity RNO 144 and the Herbig-Haro object HH 149 have not exhibited significant variation in shape and brightness during the outburst.",
keywords = "Herbig-Haro objects, ISM: individual objects (L1251), stars: formation, stars: individual: IRAS 22343 + 7501, stars: protostars, stars: variables: T Tauri, Herbig Ae/Be",
author = "M. Kun and P. {\'A}brah{\'a}m and {Acosta Pulido}, {J. A.} and A. Mo{\'o}r and T. Prusti",
year = "2019",
month = "3",
day = "11",
doi = "10.1093/mnras/sty3425",
language = "English",
volume = "483",
pages = "4424--4437",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

TY - JOUR

T1 - The outbursting protostar 2MASS 22352345 + 7517076 and its environment

AU - Kun, M.

AU - Ábrahám, P.

AU - Acosta Pulido, J. A.

AU - Moór, A.

AU - Prusti, T.

PY - 2019/3/11

Y1 - 2019/3/11

N2 - We studied the Class I protostar 2MASS 22352345 + 7517076 whose dramatic brightening between the IRAS, Akari, and WISE surveys was reported by Onozato et al. 2MASS 22352345+7517076 is a member of a small group of low-mass young stellar objects, associated with IRAS 22343 + 7501 in the molecular cloud Lynds 1251. The IRAS, ISO, Spitzer, Akari, Herschel, and WISE missions observed different stages of its outburst. Supplemented these data with archival and our own near-infrared observations, and considering the contributions of neighbouring sources to the mid-infrared fluxes we studied the nature and environment of the outbursting object, and its photometric variations from 1983 to 2017. The low-state bolometric luminosity L bol ≈32 L ⊙ is indicative of a 1.6-1.8 M⊙, 1-2 × 10 5 -yr old protostar. Its 2-μm brightness started rising between 1993 and 1998, reached a peak in 2009-2011, and started declining in 2015. Changes in the spectral energy distribution suggest that the outburst was preceded by a decade-long, slow brightening in the near-infrared. The actual accretion burst occurred between 2004 and 2007. We fitted the spectral energy distribution in the bright phases with simple accretion disc models. The modelling suggested an increase of the disc accretion rate from ~3.5 × 10 -7 M ⊙ yr -1 to ~1.1 × 10 -4 M ⊙ yr -1 . The central star accreted nearly 10 -3 M ⊙, about a Jupiter mass during the 10 yr of the outburst. We observed H 2 emission lines in the K-band spectrum during the fading phase in 2017. The associated optical nebulosity RNO 144 and the Herbig-Haro object HH 149 have not exhibited significant variation in shape and brightness during the outburst.

AB - We studied the Class I protostar 2MASS 22352345 + 7517076 whose dramatic brightening between the IRAS, Akari, and WISE surveys was reported by Onozato et al. 2MASS 22352345+7517076 is a member of a small group of low-mass young stellar objects, associated with IRAS 22343 + 7501 in the molecular cloud Lynds 1251. The IRAS, ISO, Spitzer, Akari, Herschel, and WISE missions observed different stages of its outburst. Supplemented these data with archival and our own near-infrared observations, and considering the contributions of neighbouring sources to the mid-infrared fluxes we studied the nature and environment of the outbursting object, and its photometric variations from 1983 to 2017. The low-state bolometric luminosity L bol ≈32 L ⊙ is indicative of a 1.6-1.8 M⊙, 1-2 × 10 5 -yr old protostar. Its 2-μm brightness started rising between 1993 and 1998, reached a peak in 2009-2011, and started declining in 2015. Changes in the spectral energy distribution suggest that the outburst was preceded by a decade-long, slow brightening in the near-infrared. The actual accretion burst occurred between 2004 and 2007. We fitted the spectral energy distribution in the bright phases with simple accretion disc models. The modelling suggested an increase of the disc accretion rate from ~3.5 × 10 -7 M ⊙ yr -1 to ~1.1 × 10 -4 M ⊙ yr -1 . The central star accreted nearly 10 -3 M ⊙, about a Jupiter mass during the 10 yr of the outburst. We observed H 2 emission lines in the K-band spectrum during the fading phase in 2017. The associated optical nebulosity RNO 144 and the Herbig-Haro object HH 149 have not exhibited significant variation in shape and brightness during the outburst.

KW - Herbig-Haro objects

KW - ISM: individual objects (L1251)

KW - stars: formation

KW - stars: individual: IRAS 22343 + 7501

KW - stars: protostars

KW - stars: variables: T Tauri, Herbig Ae/Be

UR - http://www.scopus.com/inward/record.url?scp=85062297529&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85062297529&partnerID=8YFLogxK

U2 - 10.1093/mnras/sty3425

DO - 10.1093/mnras/sty3425

M3 - Article

AN - SCOPUS:85062297529

VL - 483

SP - 4424

EP - 4437

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -