QW Puppis

Why is QW Puppis so important nowadays? QW Puppis has captured the attention of millions of people around the world, generating controversy and debate in all areas. Since its appearance, QW Puppis has been the subject of analysis and discussion in various fields, from science and technology to politics and popular culture. In this article we will explore the impact that QW Puppis has had on today's society and how its presence has shaped the way we think and act. Additionally, we will examine the relevance of QW Puppis in a constantly changing world and how its influence continues to be noticeable in our daily lives.

This article is about I Puppis. Not to be confused with l Puppis or j Puppis.
QW Puppis
Location of QW Puppis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension 07h 12m 33.62514s[1]
Declination −46° 45′ 33.4966″[1]
Apparent magnitude (V) 4.49[2]
Characteristics
Spectral type F3V Fe-1.0[3]
U−B color index −0.01[2]
B−V color index +0.32[2]
Variable type γ Dor[4]
Astrometry
Radial velocity (Rv)+0.10[5] km/s
Proper motion (μ) RA: −135.806[1] mas/yr
Dec.: +107.433[1] mas/yr
Parallax (π)46.9031±0.1185 mas[1]
Distance69.5 ± 0.2 ly
(21.32 ± 0.05 pc)
Absolute magnitude (MV)2.84[6]
Details
Mass1.52[7] M☉
Radius1.7[1] R☉
Luminosity6.4[7] L☉
Surface gravity (log g)4.17[8] cgs
Temperature6,934[7] K
Metallicity −0.24[6] dex
Rotational velocity (v sin i)51[7] km/s
Age1.6[1] Gyr
Other designations
I Puppis, QW Pup, CD−46°2977, FK5 275, GC 9569, GJ 268.1, GJ 9225, GSC 08119-02547, HIP 34834, HR 2740, HD 55892, SAO 218537
Database references
SIMBADdata

QW Puppis (QW Pup) is a class F3V (yellow-white dwarf) star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 69.5 light years away based on parallax.

A light curve for QW Puppis, plotted from TESS data[9]

It is a Gamma Doradus variable, ranging from 4.5 to 4.47 magnitude with a period of 0.96 days.[4] With a mass of 1.5 M☉ and an age of 1.6 billion years, it is about halfway through its main sequence lifetime.[7]

References

  1. ^ a b c d e f g 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.
  2. ^ a b c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ^ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. ^ a b Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  5. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  6. ^ 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. Vizier catalog entry
  7. ^ a b c d e Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID 55586789. Vizier catalog entry
  8. ^ 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. Vizier catalog entry
  9. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.