HD 4778

Let's talk about HD 4778. This is a topic that has captured the attention of many people in recent years. With HD 4778, numerous debates, studies and research have arisen that have tried to decipher its complexity and its impact on society. From its origins to its influence today, HD 4778 has generated unprecedented interest, being the subject of discussion in areas as diverse as politics, science, culture and everyday life. In this article, we will explore different aspects related to HD 4778, analyzing its causes, consequences and possible solutions.

HD 4778

A light curve for GO Andromedae, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 00h 50m 18.26563s[2]
Declination +45° 00′ 08.1439″[2]
Apparent magnitude (V) 6.13[3]
Characteristics
Spectral type A3VpSiSrCrEuKsn[4]
B−V color index 0.043±0.004[3]
Variable type α2 CVn[5]
Astrometry
Radial velocity (Rv)1.60[6] km/s
Proper motion (μ) RA: 65.353[2] mas/yr
Dec.: 4.133[2] mas/yr
Parallax (π)9.3224±0.0916 mas[2]
Distance350 ± 3 ly
(107 ± 1 pc)
Absolute magnitude (MV)1.18[7]
Details
Mass2.24±0.09[7] M☉
Radius2.36±0.12[8] R☉
Luminosity34.9±4.3[8] L☉
Surface gravity (log g)4.12±0.09[7] cgs
Temperature9,135±400[8] K
Rotation2.5616[7] days
Rotational velocity (v sin i)33[4] km/s
Age77[9] Myr
Other designations
GO Andromedae, BD+44° 176, FK5 2055, HD 4778, HIP 3919, HR 234, SAO 36702, PPM 43369[10]
Database references
SIMBADdata

HD 4778, also known as HR 234 and GO Andromedae, is a variable star in the constellation Andromeda. Its magnitude varies by 0.04 magnitudes from the median of 6.12 with a period of approximately 2.55 days.[11] The star is located 350 light years away, as determined from its annual parallax shift of 9.32 mas.[2]

This is an Ap star with a stellar classification of A3VpSiSrCrEuKsn,[4] showing chemical peculiarities in its spectrum from strontium, chromium, and europium.[12] It is an Alpha2 Canum Venaticorum variable[5] with a magnetic field that varies across the range +1,400 to −1,100 G.[13] This rotation-modulated variability allows direct determination of the rotation rate of 2.5616 days.[7]

HD 4778 has 2.24[7] times the mass of the Sun and 2.36[8] times the Sun's radius. The star is radiating 35[8] times the Sun's luminosity from its photosphere at an effective temperature of 9,375 K.[7] It is about 77[9] million years old.

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
  3. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  4. ^ a b c Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". Astrophysical Journal Supplement. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
  5. ^ a b Samus, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General Catalogue of Variable Stars". Astronomy Reports. GCVS 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  6. ^ Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID 119323941.
  7. ^ a b c d e f g North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, arXiv:astro-ph/9802286, Bibcode:1998A&A...334..181N
  8. ^ a b c d e Perraut, K.; et al. (October 2020), "Benchmarking the fundamental parameters of Ap stars with optical long-baseline interferometric measurements", Astronomy & Astrophysics, 642: 13, Bibcode:2020A&A...642A.101P, doi:10.1051/0004-6361/202038753, A101.
  9. ^ a b David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607.
  10. ^ "HD 3167". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 6, 2018.
  11. ^ VSX (4 January 2010). "GO Andromedae". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014.
  12. ^ Panek, R. J. (October 1980). "Periodic spectral variability of the AP star HR 234". Astronomy and Astrophysics. 90 (3): 341–343. Bibcode:1980A&A....90..341P.
  13. ^ Bohlender, D. A. (August 1989). "The magnetic field and rotation period of the AP star HD 4778". Astronomy and Astrophysics. 220: 215–217. Bibcode:1989A&A...220..215B.