Astronomy:Pi1 Ursae Majoris

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Short description: Star in the constellation Ursa Major


Pi1 Ursae Majoris
Diagram showing star positions and boundaries of the Centaurus constellation and its surroundings
Diagram showing star positions and boundaries of the Centaurus constellation and its surroundings

Location of π¹ Ursae Majoris (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ursa Major
Right ascension  08h 39m 11.70440s[1]
Declination +65° 01′ 15.2667″[1]
Apparent magnitude (V) 5.63
Characteristics
Spectral type G1.5Vb[2]
U−B color index +0.07[3]
B−V color index +0.62[3]
Variable type BY Draconis
Astrometry
Radial velocity (Rv)–13.88 ± 0.47[4] km/s
Proper motion (μ) RA: -27.44 ± 0.31[1] mas/yr
Dec.: +88.13 ± 0.26[1] mas/yr
Parallax (π)69.66 ± 0.37[1] mas
Distance46.8 ± 0.2 ly
(14.36 ± 0.08 pc)
Absolute magnitude (MV)4.86[5]
Details
Mass0.90[6] M☉
Luminosity0.97[7] L☉
Surface gravity (log g)4.48[8] cgs
Temperature5,884 ± 6.8[9] K
Metallicity [Fe/H]–0.04[8] dex
Rotation5 days[10]
Rotational velocity (v sin i)14.27[4] km/s
Age200[11] Myr
Other designations
π¹ Ursae Majoris, π¹ UMa, Pi1 UMa, 3 Ursae Majoris, BD +65°643, GC 11817, HD 72905, HIP 42438, HR 3391, PPM 16705, SAO 14609.
Database references
SIMBADdata
A light curve for pi1 Ursae Majoris, plotted from TESS data.[12] The main plot shows the variation over several weeks, and the inset plot shows the same data folded, assuming a 4.9 day period,[13] and averaged into 250 phase bins.

Pi1 Ursae Majoris (Pi1 UMa, π¹ Ursae Majoris, π¹ UMa) is a yellow G-type main sequence dwarf with a mean apparent magnitude of +5.63. It is approximately 46.8 light years from Earth,[1] and is a relatively young star with an age of about 200 million years.[11] It is classified as a BY Draconis type variable star and its brightness varies by 0.08 magnitudes. In 1986, it became the first solar-type star to have the emission from an X-ray flare observed.[14] Based upon its space velocity components, this star is a member of the Ursa Major moving group of stars that share a common motion through space.[7][10]

An excess of infrared radiation has been detected from this system, which suggests the presence of a debris disk. The best fit to the data indicates that there is a ring of fine debris out to a radius of about 0.4 AU, consisting of 0.25 μm grains of amorphous silicates or crystalline forsterite. There may also be a wider ring of larger (10 μm) grains out to a distance of 16 AU.[15]

Naming and etymology

With π2, σ1, σ2, ρ, A and d, it composed the Arabic asterism Al Ṭhibā᾽, the Gazelle.[16] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Al Ṭhibā were the title for seven stars : A as Althiba I, this star (π1) as Althiba II, π2 as Althiba III, ρ as Althiba IV, σ1 as Althiba V, σ2 as Althiba VI, and d as Althiba VII.[17]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, Floor (2007). "Hipparcos, the new Reduction of the Raw data". Astron. Astrophys. 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.  Note: see VizieR catalogue I/311.
  2. ↑ Montes, D. et al. (November 2001), "Late-type members of young stellar kinematic groups - I. Single stars", Monthly Notices of the Royal Astronomical Society 328 (1): 45–63, doi:10.1046/j.1365-8711.2001.04781.x, Bibcode: 2001MNRAS.328...45M, http://eprints.ucm.es/30941/1/castrorubio18libre.pdf, retrieved 2018-11-04 
  3. ↑ 3.0 3.1 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J 
  4. ↑ 4.0 4.1 White, Russel J.; Gabor, Jared M.; Hillenbrand, Lynne A. (June 2007), "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun", The Astronomical Journal 133 (6): 2524–2536, doi:10.1086/514336, Bibcode: 2007AJ....133.2524W 
  5. ↑ Holmberg, J. et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics 501 (3): 941–947, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H. 
  6. ↑ Shaya, Ed J.; Olling, Rob P. (January 2011), "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue", The Astrophysical Journal Supplement 192 (1): 2, doi:10.1088/0067-0049/192/1/2, Bibcode: 2011ApJS..192....2S 
  7. ↑ 7.0 7.1 Gaidos, E. J.; Henry, G. W.; Henry, S. M. (August 2000), "Spectroscopy and Photometry of Nearby Young Solar Analogs", The Astronomical Journal 120 (2): 1006–1013, doi:10.1086/301488, Bibcode: 2000AJ....120.1006G 
  8. ↑ 8.0 8.1 Cenarro, A. J. et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society 374 (2): 664–690, doi:10.1111/j.1365-2966.2006.11196.x, Bibcode: 2007MNRAS.374..664C 
  9. ↑ Kovtyukh, V. V. et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics 411 (3): 559–564, doi:10.1051/0004-6361:20031378, Bibcode: 2003A&A...411..559K 
  10. ↑ 10.0 10.1 Maldonado, J. et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics 521: A12, doi:10.1051/0004-6361/201014948, Bibcode: 2010A&A...521A..12M 
  11. ↑ 11.0 11.1 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, doi:10.1086/591785, Bibcode: 2008ApJ...687.1264M 
  12. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  13. ↑ Kochukhov, O.; Hackman, T.; Lehtinen, J. J. (March 2020). "Hidden magnetic fields of young suns". Astronomy & Astrophysics 635: A142. doi:10.1051/0004-6361/201937185. Bibcode: 2020A&A...635A.142K. https://www.aanda.org/articles/aa/pdf/2020/03/aa37185-19.pdf. Retrieved 30 June 2022. 
  14. ↑ Landini, M. et al. (March 1986), "EXOSAT detection of an X-ray flare from the solar type star Pi-prime UMa", Astronomy and Astrophysics 157 (2): 217–222, Bibcode: 1986A&A...157..217L 
  15. ↑ Beichman, C. A. et al. (2006), "IRS Spectra of Solar-Type Stars: A Search for Asteroid Belt Analogs", The Astrophysical Journal 639 (2): 1166–1176, doi:10.1086/499424, Bibcode: 2006ApJ...639.1166B 
  16. ↑ Allen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, p. 444 
  17. ↑ Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars, Jet Propulsion Laboratory, California Institute of Technology, https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19720005197_1972005197.pdf. 

External links



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