Astronomy:3 Piscis Austrini

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Short description: Star in the constellation Microscopium
3 Piscis Austrini
Microscopium constellation map.svg
Red circle.svg
Location of 3 PsA (circled)
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Microscopium
Right ascension  21h 13m 17.32730s[1]
Declination −27° 37′ 09.7106″[1]
Apparent magnitude (V) 5.39±0.01[2]
Characteristics
Spectral type K3 III[3]
B−V color index +1.42[4]
Astrometry
Radial velocity (Rv)−46.2±2.4[5] km/s
Proper motion (μ) RA: +98.513[1] mas/yr
Dec.: −110.906[1] mas/yr
Parallax (π)8.0734 ± 0.1733[1] mas
Distance404 ± 9 ly
(124 ± 3 pc)
Absolute magnitude (MV)+0.19[6]
Details
Mass1.58[7] M☉
Radius31.3±1.6[8] R☉
Luminosity184+9−8[1] L☉
Surface gravity (log g)1.86[9] cgs
Temperature4,225±123[10] K
Metallicity [Fe/H]−0.17[9] dex
Rotational velocity (v sin i)<1[11] km/s
Age2.59+0.83−1.90[1] Gyr
Other designations
3 PsA, CD−28°17178, CPD−28°7411, FK5 1556, GC 29652, HD 201901, HIP 104750, HR 8110, SAO 190129[12]
Database references
SIMBADdata

3 Piscis Austrini, also known as HD 201901 or simply 3 PsA, is an astrometric binary[13] (100% chance[14]) located in the southern constellation Microscopium. It was once part of Piscis Austrinus, the southern fish. The system has a combined apparent magnitude of 5.39,[2] making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 404 light years[1] and it is currently approaching the Solar System with a heliocentric radial velocity of −46.2 km/s.[5] At its current distance, 3 PsA's brightness is diminished by 0.12 magnitudes due to extinction from interstellar dust[15] and it has an absolute magnitude of +0.19.[6]

The visible component is an evolved red giant with a stellar classification of K3 III.[3] The interferometry-measured angular diameter of the star, after correcting for limb darkening, is 2.03±0.04 mas,[16] which, at its estimated distance, equates to a physical radius of about 20 times the radius of the Sun.[17] However, its actual empirical radius is 31.3 R☉.[8] It has 1.58 times the mass of the Sun[7] and is radiating 184 times the luminosity of the Sun[1] from its enlarged photosphere at an effective temperature of 4,225 K.[10] 3 PsA is metal deficent with an iron abundance 68% that of the Sun ([Fe/H] = −0.17)[9] and it spins too slowly for its projected rotational velocity to be measured accurately.[11] It is estimated to be 2.59 billion years old based on Gaia DR3 models.[1]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 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 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume III: Declinations −40° to −26°. Bibcode: 1982mcts.book.....H. 
  4. ↑ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory 4: 99–110. Bibcode: 1966CoLPL...4...99J. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  6. ↑ 6.0 6.1 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 Anders, F. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  8. ↑ 8.0 8.1 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants. Surface brightness relations calibrated by interferometry". Astronomy & Astrophysics 426 (1): 297–307. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  9. ↑ 9.0 9.1 9.2 McWilliam, Andrew (December 1990). "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances". The Astrophysical Journal Supplement Series 74: 1075. doi:10.1086/191527. ISSN 0067-0049. Bibcode: 1990ApJS...74.1075M. 
  10. ↑ 10.0 10.1 Stassun, Keivan G. et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S. 
  11. ↑ 11.0 11.1 De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars V: Southern stars *". Astronomy & Astrophysics 561: A126. doi:10.1051/0004-6361/201220762. ISSN 0004-6361. Bibcode: 2014A&A...561A.126D. 
  12. ↑ "HD 201901". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+201901. 
  13. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  14. ↑ Frankowski, A.; Jancart, S.; Jorissen, A. (19 December 2006). "Proper-motion binaries in the Hipparcos catalogue: Comparison with radial velocity data". Astronomy & Astrophysics 464 (1): 377–392. doi:10.1051/0004-6361:20065526. ISSN 0004-6361. Bibcode: 2007A&A...464..377F. 
  15. ↑ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society 472 (4): 3805–3820. doi:10.1093/mnras/stx2219. ISSN 0035-8711. Bibcode: 2017MNRAS.472.3805G. 
  16. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy & Astrophysics 431 (2): 773–777. doi:10.1051/0004-6361:20042039. ISSN 0004-6361. Bibcode: 2005A&A...431..773R. 
  17. ↑ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1, https://books.google.com/books?id=OvTjLcQ4MCQC&pg=PA41.  The radius (R*) is given by:
    [math]\displaystyle{ \begin{align} 2\cdot R_* & = \frac{(10^{-3}\cdot 93.6\cdot 2.03)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 40.9\cdot R_{\bigodot} \end{align} }[/math]
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