Astronomy:FU Tauri

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Short description: Star in the constellation Taurus
FU Tauri
250px
FU Tauri and its companion (lower left)
Credit: Image Credit: NASA/ESA/CSA JWST; Ya-Lin Wu et al.; processing: Meli_thev
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Taurus
A
Right ascension  04h 23m 35.391s[1]
Declination +25° 03′ 02.75″[1]
Apparent magnitude (V)
B
Right ascension  04h 23m 35.746s[2]
Declination +25° 02′ 59.64″[2]
Apparent magnitude (V)
Characteristics
A
Evolutionary stage pre-main sequence[3]
Spectral type M7.25[4]
Apparent magnitude (G) 15.23[1] + 20.45[2]
Variable type T Tau[5]
B
Evolutionary stage brown dwarf[6]
Spectral type M9.25[4]
Apparent magnitude (G) 20.45[2]
Astrometry
A
Radial velocity (Rv)+19.67±0.01[7] km/s
Proper motion (μ) RA: +6.901[1] mas/yr
Dec.: −21.252[1] mas/yr
Parallax (π)7.8354 ± 0.0754[1] mas
Distance416 ± 4 ly
(128 ± 1 pc)
B
Proper motion (μ) RA: +1.5 mas/yr
Dec.: −24.2 mas/yr
Parallax (π)7.4750 ± 1.1221[2] mas
Distanceapprox. 440 ly
(approx. 130 pc)
Details
A
Mass0.05[4] M☉
Luminosity0.2[4] L☉
Rotation3.93±0.10[8] days
Rotational velocity (v sin i)17.4±0.3[8] km/s
Age<1[4] Myr
B
Mass0.015[4] M☉
Luminosity0.039[4] L☉
Age<1[4] Myr
Other designations
Gaia DR2 149629483705467008, WDS J04236+2503A, 2MASS J04233539+2503026
Database references
SIMBADA
B

FU Tauri is a binary brown dwarf in the constellation of Taurus. Based on parallax measurements, it is about 416 light years away.

Variability

A red band light curve for FU Tauri, adapted from Scholz et al. (2012)[9]

FU Tauri varies in brightness. The primary is a T Tauri variable, a type of irregular pre-main-sequence star. Its brightness has been observed to vary from a photovisual magnitude of 16.0 to fainter than 17.0.[10] Its photographic magnitude has been measured to vary between magnitude 15.1 and below magnitude 17.6.[11]

Characteristics

The primary and secondary, FU Tauri A and B, have spectral types of M7.25 and M9.25, which are suggestive of masses of 0.05 and 0.015 solar masses (M☉)[4]. The system is very young, only ~1 million years old. Both brown dwarfs have infrared emission that indicates the presence of circumstellar disks[4]. The binary system has a projected separation of 5.7″, which is equivalent to a projected separation of 800 astronomical unit|AU at the system's distance.[1]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ Skinner, Stephen; Güdel, Manuel; Briggs, Kevin; Melnikov, Stanislav; Audard, Marc (2006). "X-ray Emission from the Pre-Main Sequence Systems FU Orionis and T Tauri". Astrophysics and Space Science 304 (1–4): 165. doi:10.1007/s10509-006-9100-5. Bibcode: 2006Ap&SS.304..165S. 
  4. ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 Luhman, K. L.; Mamajek, E. E.; Allen, P. R.; Muench, A. A.; Finkbeiner, D. P. (2009). "Discovery of a Wide Binary Brown Dwarf Born in Isolation". The Astrophysical Journal 691 (2): 1265. doi:10.1088/0004-637X/691/2/1265. Bibcode: 2009ApJ...691.1265L. 
  5. ↑ Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: B/GCVS. Bibcode: 2009yCat....102025S. 
  6. ↑ Wu, Ya-Lin; Cheng, Yu-Chi; Huang, Li-Ching; Bowler, Brendan P.; Close, Laird M.; Tseng, Wei-Ling; Chen, Ning; Chen, Da-Wei (2023-09-05). "Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B". The Astronomical Journal 166 (4): 143. doi:10.3847/1538-3881/acedb0. ISSN 0004-6256. Bibcode: 2023AJ....166..143W. 
  7. ↑ Jönsson, Henrik; Holtzman, Jon A.; Prieto, Carlos Allende; Cunha, Katia; García-Hernández, D. A.; Hasselquist, Sten; Masseron, Thomas; Osorio, Yeisson et al. (2020-08-17). "APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South". The Astronomical Journal 160 (3): 120. doi:10.3847/1538-3881/aba592. ISSN 0004-6256. Bibcode: 2020AJ....160..120J. 
  8. ↑ 8.0 8.1 Bowler, Brendan P.; Tran, Quang H.; Zhang, Zhoujian; Morgan, Marvin; Ashok, Katelyn B.; Blunt, Sarah; Bryan, Marta L.; Evans, Analis E. et al. (2023-03-17). "Rotation Periods, Inclinations, and Obliquities of Cool Stars Hosting Directly Imaged Substellar Companions: Spin–Orbit Misalignments Are Common". The Astronomical Journal 165 (4): 164. doi:10.3847/1538-3881/acbd34. ISSN 0004-6256. Bibcode: 2023AJ....165..164B. 
  9. ↑ Scholz, Alexander; Stelzer, Beate; Costigan, Grainne; Barrado, David; Eislöffel, Jochen; Lillo-Box, Jorge; Riviere-Marichalar, Pablo; Stoev, Hristo (January 2012). "Magnetic activity and accretion on FU Tau A: clues from variability". Monthly Notices of the Royal Astronomical Society 419 (2): 1271–1279. doi:10.1111/j.1365-2966.2011.19781.x. Bibcode: 2012MNRAS.419.1271S. 
  10. ↑ Romano, G. (1975). "Observations of T Tau stars and related objects in Taurus dark cloud". Memorie della Societa Astronomica Italiana 46: 81. Bibcode: 1975MmSAI..46...81R. 
  11. ↑ Gotz, W. (1961). "Photographische Untersuchungen an RW Aurigae-Sternen in den Dunkelgebieten von Taurus und Orion". Veroeffentlichungen der Sternwarte Sonneberg 5: 87. Bibcode: 1961VeSon...5...87G. 



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