| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas [3] |
| 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 | |
| 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.
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]
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]
The star is surrounded by a protoplanetary disk. The disk is strongly depleted in carbon and carbon monoxide. [14]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 0–120 [15] AU | 30 [14] ° | — | |||
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]
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ a b "V* BP Tau". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b 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, arXiv: astro-ph/0008370, Bibcode: 2000ApJ...545.1034S, doi: 10.1086/317838, S2CID 18064837
- ^ a b c d 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, Bibcode: 2001A&A...377..557E, doi: 10.1051/0004-6361:20011108
- ^ a b c d 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, arXiv: 1908.08583, Bibcode: 2019ApJ...882...75F, doi: 10.3847/1538-4357/ab35d4, S2CID 201645503
- ^ 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, arXiv: 1009.3300, doi: 10.1111/j.1365-2966.2010.18193.x, S2CID 55134816
- ^ 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, arXiv: astro-ph/0503144, Bibcode: 2005A&A...432L..35S, doi: 10.1051/0004-6361:200500014, S2CID 2457531
- ^ 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, S2CID 226236865
- ^ 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, arXiv: 0911.5455, Bibcode: 2012NewA...17..232L, doi: 10.1016/j.newast.2011.08.001, S2CID 119113916
- ^ Itoh, Yoichi; Tamura, Motohide; Hayashi, Masahiko; Oasa, Yumiko; Hayashi, Saeko S.; Fukagawa, Misato; Kudo, Tomoyuki; Mayama, Satoshi; Ishii, Miki; Pyo, Tae-Soo; Yamashita, Takuya; Morino, Junichi (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. Bibcode: 2008PASJ...60..209I. doi: 10.1093/pasj/60.2.209. hdl: 20.500.14094/90001427.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b Kama, 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. S2CID 53941444.
- ^ 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. Bibcode: 2003A&A...402.1003D. doi: 10.1051/0004-6361:20030317.
- ^ 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.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas [3] |
| 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 | |
| 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.
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]
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]
The star is surrounded by a protoplanetary disk. The disk is strongly depleted in carbon and carbon monoxide. [14]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 0–120 [15] AU | 30 [14] ° | — | |||
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]
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ a b "V* BP Tau". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b 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, arXiv: astro-ph/0008370, Bibcode: 2000ApJ...545.1034S, doi: 10.1086/317838, S2CID 18064837
- ^ a b c d 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, Bibcode: 2001A&A...377..557E, doi: 10.1051/0004-6361:20011108
- ^ a b c d 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, arXiv: 1908.08583, Bibcode: 2019ApJ...882...75F, doi: 10.3847/1538-4357/ab35d4, S2CID 201645503
- ^ 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, arXiv: 1009.3300, doi: 10.1111/j.1365-2966.2010.18193.x, S2CID 55134816
- ^ 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, arXiv: astro-ph/0503144, Bibcode: 2005A&A...432L..35S, doi: 10.1051/0004-6361:200500014, S2CID 2457531
- ^ 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, S2CID 226236865
- ^ 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, arXiv: 0911.5455, Bibcode: 2012NewA...17..232L, doi: 10.1016/j.newast.2011.08.001, S2CID 119113916
- ^ Itoh, Yoichi; Tamura, Motohide; Hayashi, Masahiko; Oasa, Yumiko; Hayashi, Saeko S.; Fukagawa, Misato; Kudo, Tomoyuki; Mayama, Satoshi; Ishii, Miki; Pyo, Tae-Soo; Yamashita, Takuya; Morino, Junichi (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. Bibcode: 2008PASJ...60..209I. doi: 10.1093/pasj/60.2.209. hdl: 20.500.14094/90001427.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b Kama, 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. S2CID 53941444.
- ^ 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. Bibcode: 2003A&A...402.1003D. doi: 10.1051/0004-6361:20030317.
- ^ 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.
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