44 Tauri

Last updated
44 Tauri
IMTauLightCurve.png
A light curve for IM Tauri, plotted from TESS data. [1] The 3.479 hour period [2] is marked in red.
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Taurus
Right ascension 04h 10m 49.86084s [3]
Declination +26° 28′ 51.4365″ [3]
Apparent magnitude  (V)5.37 - 5.58 [4]
Characteristics
Spectral type F2 IV [5]
Variable type δ Scuti [4]
Astrometry
Radial velocity (Rv)17.43±0.64 [3] km/s
Proper motion (μ)RA: −30.919±0.123 [3] mas/yr
Dec.: −35.105±0.072 [3] mas/yr
Parallax (π)15.4199±0.0863  mas [3]
Distance 212 ± 1  ly
(64.9 ± 0.4  pc)
Absolute magnitude  (MV)1.44±0.16 [6]
Details
Primary
Mass 1.89 [6]   M☉
Surface gravity (log g)3.6±0.1 [5]   cgs
Temperature 7000±200 [7]   K
Rotational velocity (v sin i)2±1 [7]  km/s
Other designations
p Tauri, IM Tauri, BD+26 411, HIP  19513, HD  26322, HR  1287, SAO  76485 [8]
Database references
SIMBAD data

44 Tauri, also known as HD 1287 and IM Tauri, is a star located about 210 light years from the Earth, in the constellation Taurus. [3] It is a 5th magnitude star, making it faintly visible to the naked eye of an observer located far from city lights. It is a Delta Scuti variable star, ranging between magnitude 5.37 and 5.58 over a period of about 3.5 hours. [4]

In 1966, Ivan Danziger and Robert Dickens discovered that 44 Tauri was a low amplitude variable star, with a period of approximately 3.22 hours. [9] In a follow-up study published the next year, they reported that the period was irregular, indicating beat phenomena, and they classified it as a δ Scuti variable. [10] In 1968, 44 Tauri was given the variable star designation IM Tauri. [11]

44 Tauri has been a popular object for detailed astroseismic and spectroscopic studies, because its very slow (relative to other δ Scuti stars) rotation speed of 3±2 km/sec does not complicate pulsation mode identification or greatly broaden spectral lines. [5] [7] [12] As of 2010, 44 Tauri had been found to pulsate with 15 independent periods, ranging from 1.89 to 4.52 hours. [5]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 16 January 2023.
  2. ↑ "IM Tau". The International Variable Star Index. AAVSO. Retrieved 19 January 2023.
  3. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  4. 1 2 3 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi: 10.1134/S1063772917010085 . S2CID   125853869.
  5. 1 2 3 4 Lenz, P.; Pamyatnykh, A. A.; Zdravkov, T.; Breger, M. (January 2010). "A δ Scuti star in the post-MS contraction phase: 44 Tauri" (PDF). Astronomy and Astrophysics. 509: A90. arXiv: 0911.4339 . Bibcode:2010A&A...509A..90L. doi:10.1051/0004-6361/200912914. S2CID   119311255 . Retrieved 19 January 2023.
  6. 1 2 Civelek, R.; Kızıloğlu, N.; Kırbıyık, H. (October 2001). "Radial and Nonradial Oscillations of 44 Tauri". The Astronomical Journal. 122 (4): 2042–2046. Bibcode:2001AJ....122.2042C. doi: 10.1086/323078 . hdl: 11511/66296 . S2CID   122087742.
  7. 1 2 3 Lenz, P.; Pamyatnykh, A. A.; Zdravkov, T.; Breger, M. (August 2007). "High-resolution spectroscopy of the δ Scuti star 44 Tauri: photospheric element abundances and mode identification" (PDF). Astronomy and Astrophysics. 471 (1): 237–245. arXiv: 0911.4339 . Bibcode:2010A&A...509A..90L. doi:10.1051/0004-6361/200912914. S2CID   119311255 . Retrieved 19 January 2023.
  8. ↑ "p Tau -- delta Sct Variable". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-01-19.
  9. ↑ Danziger, I. J.; Dickens, R. J. (August 1966). "Observations of Variable F-Type Stars with Short Periods". Information Bulletin on Variable Stars. 150: 1. Bibcode:1966IBVS..150....1D . Retrieved 19 January 2023.
  10. ↑ Danziger, I. J.; Dickens, R. J. (July 1967). "Spectrophotometry of New Short-Period Variable Stars". Astrophysical Journal. 149: 55–72. Bibcode:1967ApJ...149...55D. doi: 10.1086/149231 .
  11. ↑ Kukarkin, B. V.; Efremov, Yu. N.; Frolov, M. S.; Medvedeva, G. I.; Kholopov, P. N.; Kurochkin, N. E.; Kukarkina, N. P.; Perova, N. B.; Fedorovich, V. P. (November 1968). "Identification List of the New Variable Stars Nominated in 1968". Information Bulletin on Variable Stars. 311: 1. Bibcode:1968IBVS..311....1K . Retrieved 19 January 2023.
  12. ↑ Zima, W.; Lehmann, H.; Stütz, Ch.; Ilyin, I. V.; Breger, M. (August 2007). "High-resolution spectroscopy of the δ Scuti star 44 Tauri: photospheric element abundances and mode identification" (PDF). Astronomy and Astrophysics. 471 (1): 237–245. Bibcode:2007A&A...471..237Z. doi:10.1051/0004-6361:20077201 . Retrieved 19 January 2023.
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