19 Aquilae

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19 Aquilae
19 Aquilae, 2007-04-21.jpg
Image captured from Mount Laguna, California
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Aquila
Right ascension 19h 08m 59.90684s [1]
Declination +06° 04′ 23.4857″ [1]
Apparent magnitude  (V)5.227 [2]
Characteristics
Spectral type F0 III-IV [3]
Apparent magnitude  (U)5.59±0.010 [4]
Apparent magnitude  (B)5.57±0.007 [5]
Apparent magnitude  (V)5.23±0.009 [5]
U−B color index +0.020 [2]
B−V color index +0.345 [2]
Variable type suspected γ Dor [6]
Astrometry
Radial velocity (Rv)−46.7 [7]  km/s
Proper motion (μ)RA: −5.485 [1]   mas/yr
Dec.: −73.785 [1]   mas/yr
Parallax (π)22.9563 ± 0.2397  mas [1]
Distance 142 ± 1  ly
(43.6 ± 0.5  pc)
Absolute magnitude  (MV)1.94 [8]
Details
Mass 1.54 [9]   M☉
Radius 2.50+0.25
−0.05 [1]   R☉
Luminosity 12.8±0.2 [1]   L☉
Surface gravity (log g)4.13 [3]   cgs
Temperature 6,784±53 [9]   K
Metallicity [Fe/H]+0.03 [3]   dex
Rotational velocity (v sin i)57.0 [10]  km/s
Age 2.25 [9]   Gyr
Other designations
19 Sge, BD+5°4040, FK5  3530, HD  178596, HIP  94068, HR  7266, SAO  124318 [11]
Database references
SIMBAD data

19 Aquilae is a single [12] star located 142 light-years (44 parsecs ) away from the Sun in the equatorial constellation of Aquila. 19 Aquilae is the Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.23. [2] The star is moving closer to the Earth with a heliocentric radial velocity of −46.7 km/s. [7]

This object has a stellar classification of F0 III-IV, [3] with the luminosity class matching an evolving star transitioning from the subgiant to a giant stage. Poretti et al. (2003) list it as a suspected Gamma Doradus variable, and it is located near the cooler end of the instability strip on the Hertzsprung–Russell diagram. [6] These spatial coordinates are a source of X-ray emission, which is most likely coming from the star. [13]

19 Aquilae is an estimated 2.25 [9]  billion years old with a moderately high rate of spin, showing a projected rotational velocity of 57.0 km/s. [10] It has 1.54 [9] times the mass of the Sun and 2.50 [1] times the Sun's radius. The star is radiating 12.8 [1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,784 K. [9]

Related Research Articles

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

Lambda Aquilae, Latinized from λ Aquilae, is a star in the constellation Aquila. It has the traditional name Al Thalimain, which it shares with ι Aquilae. The name is derived from the Arabic الظلیمينal-ẓalīmayn "the two ostriches". Lambda Aquilae is more precisely Al Thalimain Prior. It has an apparent visual magnitude of 3.43, which is bright enough to be seen with the naked eye. Parallax measurements place it at a distance of about 125 light-years from Earth.

<span class="mw-page-title-main">Phi Aquilae</span> Binary star system in the constellation Aquila

Phi Aquilae, Latinized from φ Aquilae, is the Bayer designation of a binary star system in the equatorial constellation of Aquila. It has an apparent visual magnitude of +5.28 and is visible to the naked eye. With an annual parallax shift of 14.198 mas, this star is located at a distance of approximately 230 light-years from Earth. It is drifting closer with a radial velocity of –27 km/s. Based on its motion through space, this system is considered a possible member of the nearby Argus association of co-moving stars, although it may be too old.

<span class="mw-page-title-main">Sigma Arietis</span> Star in the constellation Aries

Sigma Arietis, Latinized from σ Arietis, is the Bayer designation for a star in the northern constellation of Aries. It has an apparent visual magnitude of +5.52, which is bright enough for the star to be seen with the naked eye from dark suburban skies. The star is located at a distance of approximately 470 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +17 km/s. On November 20, 1952, it was observed being occulted by the planet Jupiter.

49 Arietis is a single star in the northern constellation of Aries. 49 Arietis is the Flamsteed designation. It is visible to the naked eye as a faint, white hued star with an apparent visual magnitude of 5.90. The star is located at a distance of about 223 light-years distant from Earth based on parallax.

<span class="mw-page-title-main">26 Arietis</span> Star in the constellation Aries

26 Arietis is a variable star in the northern constellation of Aries. 26 Arietis is the Flamsteed designation; it also bears the variable star designation UU Arietis. The apparent visual magnitude of this star is 6.14, which, according to the Bortle Dark-Sky Scale, is within the naked eye visibility limit in dark rural skies. The annual parallax shift of 13.78 mas is equivalent to a distance of approximately 215 light-years from Earth. The star is receding from the Earth with a heliocentric radial velocity of +15 km/s.

11 Aquilae is a single star in the equatorial constellation of Aquila. 11 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.2, which means it is faintly visible to the naked eye. Based upon an annual parallax shift of 20.9 mas, the distance to this star is approximately 156 light-years. The brightness of this star is diminished by 0.33 in magnitude because of extinction from interstellar gas and dust.

8 Aquilae is a star in the equatorial constellation of Aquila, located 271 light years away from the Sun. 8 Aquilae is the Flamsteed designation. It can be viewed with the naked eye in good seeing conditions, appearing as a dim, yellow-white hued star with an apparent visual magnitude of 6.08. The star is moving further from the Earth with a heliocentric radial velocity of +12 km/s.

<span class="mw-page-title-main">HR 511</span> Star in the constellation Cassiopeia

HR 511 is an orange dwarf of spectral type K0V in the constellation Cassiopeia. With an apparent magnitude of 5.63, it is faintly visible to the naked eye. The star is relatively close, 32.8 light years from the Sun.

HR 5256 is a star located thirty-three light-years away from the Sun in the northern circumpolar constellation of Ursa Major. It has an orange hue and is a challenge to view with the naked eye, having an apparent visual magnitude of 6.52 The distance to this star is very nearly 10 parsecs, so the absolute magnitude of 6.51 is nearly the same as the star's apparent magnitude. HR 5256 is drifting nearer to the Sun with a radial velocity of −26.4 km/s, and will make its closest approach to the Sun in about 333,000±16,000 years, when it will be at a distance of 12.72 ± 0.65 light-years.

HD 220105 is a star in the northern constellation of Andromeda, and a member of the Sirius supercluster. It lies near the lower limit of visibility to the naked eye at an apparent visual magnitude of 6.24, and can be a challenge to spot under normal viewing conditions. The star is located 238 light years away, based upon an annual parallax shift of 13.78 mas. It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.

HD 156768 is a double star in the southern constellation of Ara, with a combined apparent magnitude of 5.86. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.

<span class="mw-page-title-main">HD 126009</span> Star in the constellation Boötes

HD 126009 or CI Boötis is a variable star in the northern constellation of Boötes.

16 Camelopardalis is a single star in the northern circumpolar constellation Camelopardalis, located 348 light years away from the Sun as determined from parallax measurements. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.28. This object is moving further from the Earth with a heliocentric radial velocity of around 12 km/s.

HD 32518 is a solitary star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 6.42, placing it near the max naked eye visibility. Located about 400 light years away, it is receding with a heliocentric radial velocity of −7.02 km/s.

<span class="mw-page-title-main">1 Camelopardalis</span> Double star system in the constellation Camelopardalis

1 Camelopardalis is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately 800 parsecs (2,600 ly) away.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

Psi2 Draconis is a solitary giant star in the northern circumpolar constellation of Draco, also designated 34 Draconis. It lies just over a degree east of the brighter Psi1 Draconis. Psi2 Draconis has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.45. It is located at a distance of 940 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −2 km/s.

Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

<span class="mw-page-title-main">BU Crucis</span> Star in the constellation Crux

BU Crucis is a variable star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

HD 119124 is a wide binary star system in the circumpolar constellation of Ursa Major. With an apparent visual magnitude of 6.3, it lies below the normal brightness limit of stars that are visible with the naked eye under most viewing conditions. An annual parallax shift of 39.24 mas for the A component provides a distance estimate of 83 light years. The pair are candidate members of the Castor Moving Group, which implies a relatively youthful age of around 200 million years. HD 119124 is moving closer to the Sun with a radial velocity of −12 km/s.

References

  1. 1 2 3 4 5 6 7 8 9 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 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 Oja, T. (1986). "UBV photometry of stars whose positions are accurately known. III". Astronomy and Astrophysics Supplement Series. 65 (2): 405–4. Bibcode:1986A&AS...65..405O.
  3. 1 2 3 4 Balachandran, Suchitra (May 1, 1990). "Lithium depletion and rotation in main-sequence stars". Astrophysical Journal, Part 1. 354: 310–332. Bibcode:1990ApJ...354..310B. doi:10.1086/168691.
  4. ↑ Oja, T. (1984). "UBV photometry of stars whose positions are accurately known". Astronomy and Astrophysics Supplement Series. 57: 357. Bibcode:1984A&AS...57..357O.
  5. 1 2 Oja, T. (September 1993). "UBV photometry of stars whose positions are accurately known. VII". Astronomy and Astrophysics Supplement Series. 100 (3): 591–592. Bibcode:1993A&AS..100..591O. ISSN   0365-0138.
  6. 1 2 Poretti, E.; et al. (2003). "Preparing the COROT space mission: Incidence and characterisation of pulsation in the lower instability strip". Astronomy and Astrophysics. 406: 203–211. arXiv: astro-ph/0304422 . Bibcode:2003A&A...406..203P. doi:10.1051/0004-6361:20030711. S2CID   13047725.
  7. 1 2 Wielen, R.; et al. (1999). "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions". Veröffentlichungen Astronomisches Rechen-Institut Heidelberg. Astronomisches Rechen-Institut Heidelberg. 35 (35): 1. Bibcode:1999VeARI..35....1W.
  8. ↑ Holmberg, J.; et al. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics. 501 (3): 941–947. arXiv: 0811.3982 . Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. S2CID   118577511.
  9. 1 2 3 4 5 6 Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". Astronomical Journal. 150 (3): 88. arXiv: 1507.01466 . Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID   118505114.
  10. 1 2 Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi: 10.1051/0004-6361:200810377 [ permanent dead link ]
  11. ↑ "19 Aql". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-05-30.
  12. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  13. ↑ Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009). "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources". The Astrophysical Journal Supplement. 184 (1): 138–151. arXiv: 0910.3229 . Bibcode:2009ApJS..184..138H. doi:10.1088/0067-0049/184/1/138. S2CID   119267456.
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