Individual outbursting young stars are important laboratories for studying the physics of episodic accretion and the extent to which this phenomenon can explain the luminosity distribution of protostars .
We present new and archival data for V2775 Ori ( HOPS 223 ) , a protostar in the L 1641 region of the Orion molecular clouds that was discovered by Caratti o Garatti et al .
( 2011 ) to have recently undergone an order-of-magnitude increase in luminosity .
Our near-infrared spectra of the source have strong blueshifted He i \lambda 10830 absorption , strong H _ { 2 } O and CO absorption , and no H i emission , all typical of FU Orionis sources .
With data from IRTF , 2MASS , HST , Spitzer , WISE , Herschel , and APEX that span from 1 to 70 µm pre-outburst and from 1 to 870 µm post-outburst , we estimate that the outburst began between 2005 April and 2007 March .
We also model the pre- and post-outburst spectral energy distributions of the source , finding it to be in the late stages of accreting its envelope with a disk-to-star accretion rate that increased from \sim 2 \times 10 ^ { -6 } ~ { } M _ { \sun } ~ { } yr ^ { -1 } to \sim 10 ^ { -5 } ~ { } M _ { \sun } ~ { } yr ^ { -1 } during the outburst .
The post-outburst luminosity at the epoch of the FU Orionis-like near-IR spectra is 28 ~ { } L _ { \sun } , making V2775 Ori the least luminous documented FU Orionis outburster with a protostellar envelope .
The existence of low-luminosity outbursts supports the notion that a range of episiodic accretion phenomena can partially explain the observed spread in protostellar luminosities .