BP Tauri

Short description: Star in the constellation Taurus

Coordinates:  04h 19m 15.8343s, +29° 06′ 26.9295″

BP Tauri

250px
A light curve for BP Tauri, plotted from TESS data[1]

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Taurus
Right ascension |  04h 19m 15.8343s[2]
Declination | +29° 06′ 26.9295″[2]
Apparent magnitude (V) | 12.12
Characteristics
Evolutionary stage | pre-main-sequence star
Spectral type | K5
Apparent magnitude (G) | 11.460[3]
Variable type | T Tau
Astrometry
Radial velocity (Rv)| 15.76±0.13 km/s
Proper motion (μ)|  RA: 8.889[3] mas/yr
Dec.: -26.011[3] mas/yr
Parallax (π)| 7.8494 ± 0.0362[3] mas
Distance| 416 ± 2 ly
(127.4 ± 0.6 pc)
Details
Mass| 1.24+0.25−0.32[4] M☉
Radius| 2.0[5] R☉
Luminosity| 0.93[5] L☉
Surface gravity (log g)| 4.32±0.14[6] cgs
Temperature| 3640+94−92[6] K
Rotational velocity (v sin i)| 11.4+0.25−0.55[6] km/s
Age| 6±4[4] Myr
Other designations

Gaia DR2 164832740220756608, HD 281934, HIP 20160, TYC 1827-554-1, GSC 01827-00554, 2MASS J04191583+2906269

Database references
SIMBAD| data

BP Tauri is a young T Tauri star in the constellation of Taurus about 416 light years away, belonging to the Taurus Molecular Cloud.

## Contents

* 1 Properties
* 2 Suspected companions
* 3 Protoplanetary system
* 4 Variability
* 5 References

## Properties

BP Tauri is still accreting mass at the low rate of 9×10−10 M☉ and 1.6×10−7 M☉/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 by accretion.[5]

## Suspected companions

There were two suspected stellar companions to BP Tauri on projected separations 3.00 and 5.45 arcseconds.[11] These were proven to be a background stars not related to BP Tauri with Gaia data though.[12][13]

## Protoplanetary system

The star is surrounded by a protoplanetary disk. The disk is strongly depleted in carbon and carbon monoxide.[14]

The planetary system  Companion
(in order from star) | Mass | Semimajor axis
(AU) | Orbital period
(days) | Eccentricity | Inclination | Radius

|
|
|
|
|
|

protoplanetary disk | 0-120[15] AU | 30[14]° | —

## Variability

In 1935, Inna N. Lehmann-Balanowskaja discovered that BP Tauri is a variable star.[16] Its variation in brightness is caused by strong flares due to unsteady accretion[5] held by the stellar magnetic field. The lightcurve period is variable from 6.1 to 7.6 days, and quiescent periods without variability are also known.[17]

## References

1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
2. ↑ 2.0 2.1 "V* BP Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V*+BP+Tau.
3. ↑ 3.0 3.1 3.2 3.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
4. ↑ 4.0 4.1 Simon, M.; Dutrey, A.; Guilloteau, S. (2000), "Dynamical Masses of T Tauri Stars and Calibration of Pre–Main-Sequence Evolution", The Astrophysical Journal 545 (2): 1034–1043, doi:10.1086/317838, Bibcode: 2000ApJ...545.1034S
5. ↑ 5.0 5.1 5.2 5.3 Errico, L.; Lamzin, S. A.; Vittone, A. A. (2001), "UV spectra of T Tauri stars from the HST and IUE satellites: BP Tau", Astronomy & Astrophysics 377 (2): 557–565, doi:10.1051/0004-6361:20011108, Bibcode: 2001A&A...377..557E
6. ↑ 6.0 6.1 6.2 6.3 Flores, C.; Connelley, M. S.; Reipurth, B.; Boogert, A. (2019), "Measuring the Magnetic Field of Young Stars Using iSHELL Observations: BP Tau and V347 Aur", The Astrophysical Journal 882 (2): 75, doi:10.3847/1538-4357/ab35d4, Bibcode: 2019ApJ...882...75F
7. ↑ Long, M.; Romanova, M. M.; Kulkarni, A. K.; Donati, J.-F. (2010), "Global 3D simulations of disc accretion on to the classical T Tauri star BP Tauri", Monthly Notices of the Royal Astronomical Society 413 (2): 1061–1071, doi:10.1111/j.1365-2966.2010.18193.x
8. ↑ Schmitt, J. H. M. M.; Robrade, J.; Ness, J.-U.; Favata, F.; Stelzer, B. (2005), "X-rays from accretion shocks in T Tauri stars: The case of BP Tau", Astronomy & Astrophysics 432 (2): L35–L38, doi:10.1051/0004-6361:200500014, Bibcode: 2005A&A...432L..35S
9. ↑ 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, doi:10.3847/1538-4357/abc828
10. ↑ Long, Min; Romanova, Marina M.; Lamb, Frederick K. (2009), "Accretion onto stars with octupole magnetic fields: Matter flow, hot spots and phase shifts", New Astronomy 17 (2): 232–245, doi:10.1016/j.newast.2011.08.001, Bibcode: 2012NewA...17..232L
11. ↑ Itoh, Yoichi; Tamura, Motohide; Hayashi, Masahiko; Oasa, Yumiko; Hayashi, Saeko S.; Fukagawa, Misato; Kudo, Tomoyuki; Mayama, Satoshi et al. (2008). "Near-Infrared Spectroscopy of Faint Companions around Young Stellar Objects Associated with the Taurus Molecular Cloud". Publications of the Astronomical Society of Japan 60 (2): 209–218. doi:10.1093/pasj/60.2.209. Bibcode: 2008PASJ...60..209I.
12. ↑ Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
13. ↑ Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
14. ↑ 14.0 14.1 Kama, M.; Bruderer, S.; Carney, M.; Hogerheijde, M.; Van Dishoeck, E. F.; Fedele, D.; Baryshev, A.; Boland, W. et al. (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. doi:10.1051/0004-6361/201526791. Bibcode: 2016A&A...588A.108K.
15. ↑ Dutrey, A.; Guilloteau, S.; Simon, M. (2003). "The BP Tau disk: A missing link between Class II and III objects?". Astronomy and Astrophysics 402 (3): 1003. doi:10.1051/0004-6361:20030317. Bibcode: 2003A&A...402.1003D.
16. ↑ Burlak, M. A.; Grankin, K. N.; Dodin, A. V.; Zharova, A. V.; Ikonnikova, N. P.; Kiryukhina, V. A.; Lamzin, S. A.; Safonov, B. S. et al. (June 2025). "On the Causes of Brightness Variability of a Young Star BP Tau". Astrophysical Bulletin 80 (2): 279-293. doi:10.1134/S1990341325600255. Bibcode: 2025AstBu..80..279B. https://link.springer.com/article/10.1134/S1990341325600255. Retrieved 11 September 2025.
17. ↑ 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. doi:10.1086/115651. Bibcode: 1990AJ....100.1957S.

* v
* t
* e

Stars of Taurus

Bayer|

* α (Aldebaran)
* β (Elnath)
* γ (Prima Hyadum)
* δ1 (Secunda Hyadum)
* δ2
* δ3
* ε (Ain)
* ζ (Tianguan)
* η (Alcyone)
* θ1
* θ2
* ι
* κ1
* κ2
* λ
* μ
* ν
* ξ
* ο
* π
* ρ
* σ1
* σ2
* τ
* υ
* φ
* χ
* ψ
* ω1
* ω2

Flamsteed|

* 4 (s)
* 5 (f)
* 6 (t)
* 7
* 9
* 10
* 11
* 12
* 13
* 14
* 16 (Celaeno)
* 17 (Electra)
* 18
* 19 (Taygeta)
* 20 (Maia)
* 21 (Asterope)
* 22 (Asterope II)
* 23 (Merope)
* 24
* 26
* 27 (Atlas)
* 28 (Pleione)
* 29 (u)
* 30 (e)
* 31
* 32
* 33
* 36
* 37 (A1)
* 39 (A2)
* 40
* 41
* 44 (p)
* 45
* 46
* 47
* 48
* 51
* 53
* 55
* 56
* 57 (h)
* 58
* 60
* 62
* 63
* 66 (r)
* 70
* 71
* 72
* 75
* 76
* 79 (b)
* 80
* 81
* 83
* 84
* 85
* 88 (d)
* 89
* 90 (c)
* 93
* 95
* 96
* 97 (i)
* 98 (k)
* 99
* 101
* 103
* 104 (m)
* 105
* 106 (i)
* 107
* 108
* 109 (n)
* 110
* 111
* 113
* 114 (o)
* 115
* 116
* 117
* 118
* 119
* 120
* 121
* 122
* 125
* 126
* 127
* 128
* 129
* 130
* 131
* 132
* 133
* 134
* 135
* 136
* 137
* 139
* 140
* 44 Eri
* 49 Eri

Variable|

* T
* Y
* Z
* RR
* RV
* RW
* RY
* RZ
* SU
* SV
* SZ
* TU
* UX
* UZ
* VY
* XX
* XZ
* AA
* AH
* BP
* CD
* CI
* CQ
* CT
* CU
* CW
* CY
* DD
* DF
* DG
* DH
* DI
* DL
* DM
* DN
* DO
* DQ
* DR
* DS
* EQ
* EU
* FN
* FS
* FV
* GG
* GI
* GK
* GV
* HK
* HL
* HU
* IK
* V410
* V471
* V473
* V479
* V534
* V624
* V647
* V650
* V710
* V711
* V731
* V766
* V773
* V774
* V781
* V807
* V818
* V819
* V826
* V827
* V827
* V830
* V833
* V834
* V836
* V837
* V892
* V987
* V1038
* V1062
* V1116
* V1137
* V1141
* V1143
* V1156
* V1187
* V1229
* V1232
* V1241 (WX Eri)

HR|

* 1023
* 1028
* 1039
* 1067
* 1085
* 1089
* 1102
* 1103
* 1110
* 1119
* 1137
* 1159
* 1172
* 1183
* 1185
* 1188
* 1201
* 1222
* 1224
* 1233
* 1237
* 1238
* 1253
* 1254
* 1257
* 1279
* 1280
* 1284
* 1295
* 1307
* 1310
* 1315
* 1349
* 1354
* 1358
* 1360
* 1370
* 1385
* 1400
* 1402
* 1403
* 1406
* 1413
* 1425
* 1427
* 1436
* 1442
* 1445
* 1446
* 1448
* 1455
* 1477
* 1480
* 1490
* 1512
* 1517
* 1554
* 1566
* 1575
* 1585
* 1633
* 1642
* 1741
* 1750
* 1755
* 1831
* 1847
* 1860
* 1878
* 1902
* 1921
* 1929
* 1954
* 1997
* 2013
* 2074

HD|

* 21032
* 21585
* 23514
* 23712
* 24040
* 24368
* 24496
* 26292
* 27860
* 28086
* 28375
* 28678
* 29627
* 29647
* 36112
* 37124
* 38263
* 38524
* 285507

Gliese|

* Gliese 176

Other|

* 2MASS J03552337+1133437
* 2MASS J04414489+2301513
* A0535+26
* BD +24 692
* Butterfly star
* CoKu Tau/4
* Crab Pulsar
* Elias 16
* Elias 18
* GD 71
* Haro 6-37
* HBC 379
* HH 30
* HII 686
* HII 1306
* HII 1883
* HII 3163
* HL Tau 76
* HP Tau/G2
* Hubble I 4
* HZ 9
* IRAS 04239+2436
* IRAS 04248+2612
* IRAS 04325+2402
* IRAS 04381+2540
* L1489 IRS
* L1527
* L1551 IRS 5
* L1521F-IRS
* LkCa 15
* MWC 480
* PSR B0525+21
* PSR B0540+23
* PSR J0348+0432
* PSR J0538+2813
* Teide 1
* TMR-1
* TMC-1A
* WD 0346+246
* WISE 0410+1502

* List

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