15 Vulpeculae

Last updated
15 Vulpeculae
Vulpecula constellation map.svg
Red circle.svg
Location of 15 Vulpeculae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Vulpecula
Right ascension 20h 01m 06.0486s [1]
Declination +27° 45 12.863 [1]
Apparent magnitude  (V)4.66 [2] (4.62 - 4.67) [3]
Characteristics
Spectral type A4IIIm [3] or kA5hA7mA7 (IV–V) [4]
U−B color index +0.15 [5]
B−V color index +0.18 [5]
Variable type α2 CVn [3]
Astrometry
Radial velocity (Rv)−26.10 [6]  km/s
Proper motion (μ)RA: 57.817±0.081 [1]   mas/yr
Dec.: 3.994±0.085 [1]   mas/yr
Parallax (π)13.4427 ± 0.1050  mas [1]
Distance 243 ± 2  ly
(74.4 ± 0.6  pc)
Absolute magnitude  (MV)0.36 [2]
Details
Luminosity 59.76 [2]   L
Surface gravity (log g)3.45 [4]   cgs
Temperature 8,084 [7]   K
Metallicity [Fe/H]+0.02 [2]   dex
Rotational velocity (v sin i)15.0 [8]  km/s
Other designations
15 Vul, NT Vul, BD+27°3587, FK5  1523, GC  27753, HD  189849, HIP  98543, HR  7653, SAO  88071 [9]
Database references
SIMBAD data

15 Vulpeculae is a variable star in the northern constellation of Vulpecula, located approximately 243 light years away based on parallax. [1] It has the variable star designation NT Vulpeculae; 15 Vulpeculae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66. [2] This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s. [6]

An ultraviolet band light curve for NT Vulpeculae, adapted from Kuvshinov et al. (1976) NTVulLightCurve.png
An ultraviolet band light curve for NT Vulpeculae, adapted from Kuvshinov et al. (1976)

This is an Am star with a stellar classification of A4 IIIm, [3] matching an evolved A-type giant star. However, Gray & Garrison (1989) found a class of kA5hA7mA7 (IV–V), [4] which matches a blend of subgiant and main sequence luminosity classes with the K-line (kA5) of an A5 star and the hydrogen (hA7) and metal (mA7) absorption lines of an A7 star. It is an Alpha2 Canum Venaticorum-type variable with magnitude ranging from 4.62 down to 4.67 over a period of 14 days. [3] The star is radiating 60 [2] times the Sun's luminosity from its photosphere at an effective temperature of 8,084 K. [7]

Related Research Articles

<span class="mw-page-title-main">Alpha Vulpeculae</span> Star in the constellation Vulpecula

Alpha Vulpeculae, officially named Anser, is the brightest star in the constellation of Vulpecula. It is approximately 291 light-years from Earth. It forms a wide optical binary with 8 Vulpeculae.

<span class="mw-page-title-main">31 Vulpeculae</span> Star in the constellation Vulpecula

31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s.

<span class="mw-page-title-main">13 Vulpeculae</span> Star in the constellation Vulpecula

13 Vulpeculae is a blue giant with a stellar classification of class B9.5III in the northern constellation Vulpecula. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.57 and it is approximately 339 light years away from the Sun based on parallax. The star is radiating 180 times the luminosity of the Sun from its photosphere at an effective temperature of 8,801 K.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

<span class="mw-page-title-main">9 Vulpeculae</span> Star in the constellation Vulpecula

9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.

<span class="mw-page-title-main">Xi Leonis</span> Star in the constellation Leo

Xi Leonis is a solitary star in the zodiac constellation of Leo. It has an apparent visual magnitude of 5.0 and is faintly visible to the naked eye. The distance to this star, as determined by parallax measurements, is roughly 229 light years.

<span class="mw-page-title-main">V381 Cephei</span> Triple star system in the constellation Cepheus

V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

<span class="mw-page-title-main">Zeta Chamaeleontis</span> Variable star in the constellation Chamaeleon

Zeta Chamaeleontis, Latinized from ζ Chamaeleontis, is a star located in the constellation Chamaeleon. Located around 540 light-years distant, it shines with a luminosity approximately 522 times that of the Sun and has a surface temperature of 15,655 K.

<span class="mw-page-title-main">HD 102839</span> Star in the constellation Musca

HD 102839 is a class G6Ib star in the constellation Musca. Its apparent magnitude is 4.98 and it is approximately 1,550 light years away from Earth based on parallax.

<span class="mw-page-title-main">Zeta Pavonis</span> Star in the constellation Pavo

Zeta Pavonis, Latinized from ζ Pavonis, is an orange-hued star in the southern constellation Pavo. Its apparent magnitude is 4.01, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of this star is 14.93 mas as seen from Earth, which provides a distance estimate of approximately 420 light-years away from the Sun. It is moving closer to the Sun with a radial velocity of −16.30. Based upon its motion through space, this star appears to be a member of the Hyades Supercluster.

<span class="mw-page-title-main">Lambda Pavonis</span> Star in the constellation Pavo

λ Pavonis, Latinized as Lambda Pavonis, is a single, variable star in the southern constellation of Pavo. It is a blue-white hued star that is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.22. This object is located approximately 1,400 light years from the Sun, based upon parallax. It is a member of the Scorpius–Centaurus association.

<span class="mw-page-title-main">Pi Pavonis</span> Astrometric binary star system in the constellation Pavo

π Pavonis, Latinized as Pi Pavonis, is a candidate astrometric binary star system in the constellation Pavo. It is a white-hued star that is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.33. The distance to this object is 130 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.6 km/s.

Phi<sup>1</sup> Pavonis Single star in the constellation Pavo

Phi1 Pavonis, latinized from φ1 Pavonis, is a single star in the southern constellation of Pavo. It has a yellow-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.75. The star is located at a distance of approximately 92 light years away based on parallax. It is drifting closer to the Sun with a radial velocity of −20 km/s.

<span class="mw-page-title-main">Rho Pavonis</span> Variable star in the constellation Pavo

Rho Pavonis, Latinized from ρ Pavonis, is a single, variable star in the southern constellation of Pavo. It is yellow-white in hue and faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.86. The star is located at a distance of approximately 190 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s. It is a candidate outlying member of the Tucana Association of co-moving stars.

<span class="mw-page-title-main">V Puppis</span> Variable star in the constellation Puppis

V Puppis is a star system in the constellation Puppis. Its apparent magnitude is 4.41. There is a binary star system at the center with a B1 dwarf orbiting a B3 subgiant star. They have an orbital period of 1.45 days and a distance of only 15 solar radii apart. However, the system moves back and forth, indicating that there is a massive object orbiting them with a period around 5.47 years. Based on the mass of the object, its lack of a visible spectrum, and circumstellar matter in the system with many heavy elements, it is probably a black hole. However, a follow-up study could not confirm this object, but found signs that there may be a third object which is fainter than the other components.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

<span class="mw-page-title-main">1 Puppis</span> Star in the constellation Puppis

1 Puppis is a single star in the southern constellation of Puppis. It lies in the northern part of the constellation at a distance of about 790 ly, east of Aludra in Canis Major and just north of the white supergiant, 3 Puppis. This object is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.59. It is moving further from the Earth with a heliocentric radial velocity of +32.4 km/s.

<span class="mw-page-title-main">HD 59890</span> Star in the constellation Puppis

HD 59890 is a class G3Ib yellow supergiant star in the constellation Puppis. Its apparent magnitude is 4.65 and it is approximately 1,360 light years away based on parallax.

<span class="mw-page-title-main">HD 54893</span> Star in the constellation Puppis

HD 54893, often called A Puppis is a suspected variable star in the constellation Puppis. Its apparent magnitude is 4.83 and is approximately 860 light years away based on parallax.

<span class="mw-page-title-main">21 Sagittarii</span> Binary star system in the constellation Sagittarius

21 Sagittarii is a binary star system in the southern zodiac constellation of Sagittarius. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.81. The system is located approximately 410 light years away from the Sun based on parallax. It is moving closer to the Earth with a heliocentric radial velocity of −11.80 km/s.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 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
  3. 1 2 3 4 5 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. 1 2 3 Çay, İpek H.; Teker Yelkenci, Aysegul; Adelman, Saul J. (May 2016). "Elemental Abundance Analyses with DAO Spectrograms. XXXIX. The Am Stars 2 UMa and 15 Vul". Publications of the Astronomical Society of the Pacific. 128 (963): 054201. Bibcode:2016PASP..128e4201C. doi:10.1088/1538-3873/128/963/054201. S2CID   123542297.
  5. 1 2 Mermilliod, J. C. (2006). "VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991)". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie. 2168. Bibcode:2006yCat.2168....0M. Vizier catalog entry
  6. 1 2 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.
  7. 1 2 McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–357. arXiv: 1208.2037 . Bibcode:2012MNRAS.427..343M. doi: 10.1111/j.1365-2966.2012.21873.x . S2CID   118665352. Vizier catalog entry
  8. Glebocki, R.; Gnacinski, P. (2005). "VizieR Online Data Catalog: Catalog of Stellar Rotational Velocities (Glebocki+ 2005)". VizieR On-line Data Catalog: III/244. Originally Published in: 2005csss...13..571G; 2005yCat.3244....0G. 3244. Bibcode:2005yCat.3244....0G. Vizier catalog entry
  9. "15 Vul". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-03-15.
  10. Kuvshinov, V. M.; Hildebrandt, G.; Schoeneich, W. (January 1976). "Photoelektrische Untersuchungen des Magnetfeldes und der Helligkeit der Am-Sterne 15 VUL und 68 Tau". Astronomische Nachrichten. 297 (4): 181–188. Bibcode:1976AN....297..181K. doi:10.1002/asna.19762970405 . Retrieved 26 May 2022.