BP Tauri is still accreting mass at the low rate of9×10−10M☉ and1.6×10−7M☉/year,[7] as evidenced by X-rays produced by infalling matter,[8] and may be still in the process of spin-up.[9] Its chromospheric magnetic fields are rather strong at 2.5+0.15 −0.16 kilogauss,[6] and contains strong non-dipole components.[10] The star is producing 40% of its luminosity via the energy released byaccretion.[5]
There were two suspected stellar companions to BP Tauri on projected separations 3.00 and5.45 arcseconds.[11] These were proven to be a background stars not related to BP Tauri withGaia data though.[12][13]
BP Tauri varies in brightness, producing a strong flares due to unsteady accretion[5] held by stellar magnetic field. The lightcurve period is variable from 6.1 to 7.6 days, and quiescent periods without variability are also known.[16]
^Ireland, Lewis G.; Zanni, Claudio; Matt, Sean P.; Pantolmos, George (2020), "Magnetic Braking of Accreting T Tauri Stars: Effects of Mass Accretion Rate, Rotation, and Dipolar Field Strength",The Astrophysical Journal,906: 4,arXiv:2011.01087,doi:10.3847/1538-4357/abc828,S2CID226236865
^abKama, M.; Bruderer, S.; Carney, M.; Hogerheijde, M.; Van Dishoeck, E. F.; Fedele, D.; Baryshev, A.; Boland, W.; Güsten, R.; Aikutalp, A.; Choi, Y.; Endo, A.; Frieswijk, W.; Karska, A.; Klaassen, P.; Koumpia, E.; Kristensen, L.; Leurini, S.; Nagy, Z.; Perez Beaupuits, J. -P.; Risacher, C.; Van Der Marel, N.; Van Kempen, T. A.; Van Weeren, R. J.; Wyrowski, F.; Yıldız, U. A. (2016). "Observations and modelling of CO and [C I] in protoplanetary disks. First detections of [C I] and constraints on the carbon abundance".Astronomy and Astrophysics.588: 588.arXiv:1601.01449.Bibcode:2016A&A...588A.108K.doi:10.1051/0004-6361/201526791.S2CID53941444.
^Simon, Theodore; Vrba, Frederick J.; Herbst, William (1990). "The Ultraviolet and Visible Light Variability of BP Tauri: Possible Clues for the Origin of T Tauri Star Activity".The Astronomical Journal.100: 1957.Bibcode:1990AJ....100.1957S.doi:10.1086/115651.
