The outbursting protostar 2MASS~22352345+7517076 and its environment. (arXiv:1812.06137v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kun_M/0/1/0/all/0/1">Maria Kun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_P/0/1/0/all/0/1">Peter Abraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pulido_J/0/1/0/all/0/1">Jose Antonio Acosta Pulido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moor_A/0/1/0/all/0/1">Attila Moor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prusti_T/0/1/0/all/0/1">Timo Prusti</a>
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. (2015). 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 Lbol ~ 32 Lsun is indicative of a
100000-200000 years old protostar of 1.6-1.8 solar masses. Its 2-micron
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 some 3.5times 10^{-7} Msun yr^{-1} to 1.1 times 10^{-4}
Msun yr^{-1}. The central star accreted nearly 10^{-3} solar masses, about a
Jupiter mass during the ten years 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.
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. (2015). 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 Lbol ~ 32 Lsun is indicative of a
100000-200000 years old protostar of 1.6-1.8 solar masses. Its 2-micron
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 some 3.5times 10^{-7} Msun yr^{-1} to 1.1 times 10^{-4}
Msun yr^{-1}. The central star accreted nearly 10^{-3} solar masses, about a
Jupiter mass during the ten years 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.
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