We studied the Class I protostar 2MASS 22352345+7517076 whose dramatic brightening between the IRAS , Akari and WISE surveys was reported by .
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 _ { \mathrm { bol } } \approx 32 L _ { \sun } is indicative of a 1.6–1.8 M _ { \sun } , 1–2 \times 10 ^ { 5 } years old protostar .
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 \sim 3.5 \times 10 ^ { -7 } M _ { \sun } yr ^ { -1 } to \sim 1.1 \times 10 ^ { -4 } M _ { \sun } yr ^ { -1 } .
The central star accreted nearly 10 ^ { -3 } M _ { \sun } , 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 .