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S Normae

The topic of S Normae is a topic of great relevance in today's society. This is an issue that affects a large number of people, and that arouses great interest and concern in the population. It is a topic that has been the subject of numerous studies, research and debates in recent years, demonstrating its importance and the need to address it appropriately. In this article, we will analyze S Normae in depth, exploring its causes, consequences and possible solutions, with the aim of offering a broad and complete vision of this very relevant topic.

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S Normae
Location of S Normae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Norma
Right ascension 16h 18m 51.8325s[1]
Declination −57° 53′ 59.244″[1]
Apparent magnitude (V) 6.394[2] (6.12 - 6.77[3])
Characteristics
Spectral type F8-G0Ib[3] + B9.5V[4]
U−B color index +0.66[5]
B−V color index +1.00[5]
Variable type δ Cepheid[3]
Astrometry
Radial velocity (Rv)5.83[6] km/s
Proper motion (μ) RA: 0.07[1] mas/yr
Dec.: 0.04[1] mas/yr
Parallax (π)1.16±0.76 mas[1]
Distance924[2] pc
Absolute magnitude (MV)-4.02[4]
Orbit[4]
Period (P)8,660 yr
Semi-major axis (a)794 AU
Details[4]
Mass6.3 M☉
Radius65.6[2] R☉
Luminosity3,630 L☉
Temperature6,350 K
Metallicity+0.10[7]
companion
Mass2.4 M☉
Age80[8] Myr
Other designations
S Nor, HR 6062, SAO 243586, CD−57°6342, GSC 08719-00158, HD 146323, NGC 6087 132, GC 21898, HIP 79932, NGC 6087 155
Database references
SIMBADdata
S Normae is the brightest member of the open cluster NGC 6087.

S Normae (S Nor) is a yellow supergiant variable star in the constellation Norma. It is the brightest member of the open cluster NGC 6087.

S Normae is a Classical Cepheid variable with a visual magnitude range of 6.12 to 6.77 and a period of 9.75411 days. The spectral type varies during the pulsation cycle from F8 to G0. Its mass has been measured at 6.3 M☉ with reference to a close orbital companion, and it is over 3,000 times as luminous as the sun.

Companions

S Normae system, showing the "spectroscopic" companion and the three faint nearby companions, but not TYC 8719-794-1

S Normae is a spectroscopic binary, although the companion has now been resolved using the Hubble Space Telescope Wide Field Camera 3. The separation was 0.90" in April 2011, corresponding to 817 AU. This gives the rare opportunity for a direct determination of the mass of a Cepheid variable star and confirmation of other properties. It is a supergiant that is 6.3 times as massive as the Sun and 2,800 times as luminous. The companion a 2.4 M☉ blue-white main sequence star of spectral type B9.5.[4]

A light curve for S Normae, plotted from TESS data[9]

There is a more distant 10th magnitude companion at 30", unsurprising in the centre of an open cluster. It is TYC 8719-794-1, a chemically peculiar A or B class star. Three fainter companions have also been found: a 14th magnitude star at 14"; and two 16th magnitude stars at 20".[10]

References

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c Moskalik, P.; Gorynya, N. A. (2005). "Mean Angular Diameters and Angular Diameter Amplitudes of Bright Cepheids". Acta Astronomica. 55: 247. arXiv:astro-ph/0507076. Bibcode:2005AcA....55..247M.
  3. ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. ^ a b c d e Evans, Nancy Remage; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; Karovska, Margarita; Tingle, Evan (2013). "Binary Cepheids: Separations and Mass Ratios in 5M ⊙ Binaries". Astronomical Journal. 146 (4): 93, 10 pp. arXiv:1307.7123. Bibcode:2013AJ....146...93E. doi:10.1088/0004-6256/146/4/93. S2CID 34133110.
  5. ^ a b 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.
  6. ^ Mermilliod, J. C.; Mayor, M.; Udry, S. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy and Astrophysics. 485 (1): 303–314. Bibcode:2008A&A...485..303M. CiteSeerX 10.1.1.30.7545. doi:10.1051/0004-6361:200809664.
  7. ^ Klagyivik, P.; Szabados, L. (2009). "Observational studies of Cepheid amplitudes. I. Period-amplitude relationships for Galactic Cepheids and interrelation of amplitudes". Astronomy and Astrophysics. 504 (3): 959. arXiv:0908.3561. Bibcode:2009A&A...504..959K. doi:10.1051/0004-6361/200811464. S2CID 18283579.
  8. ^ Netopil, M.; Paunzen, E.; Heiter, U.; Soubiran, C. (2016). "On the metallicity of open clusters. III. Homogenised sample". Astronomy & Astrophysics. 585: A150. arXiv:1511.08884. Bibcode:2016A&A...585A.150N. doi:10.1051/0004-6361/201526370. S2CID 118382876.
  9. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  10. ^ Evans, Nancy Remage; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; Tingle, Evan; Karovska, Margarita; Pillitteri, Ignazio (2016). "Hubble Space Telescopesnapshot Survey for Resolved Companions of Galactic Cepheids". The Astronomical Journal. 151 (5): 129. arXiv:1603.02224. Bibcode:2016AJ....151..129E. doi:10.3847/0004-6256/151/5/129. S2CID 119248298.
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