53 Aquarii

Last updated
53 Aquarii
Aquarius IAU.svg
Cercle rouge 100%25.svg
Location of 53 Aquarii (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Aquarius
Right ascension 22h 26m 34.2753s [1]
Declination –16° 44′ 31.697″ [1]
Apparent magnitude  (V)5.56 [2] (6.35/6.57) [3]
Characteristics
Spectral type G1 V + G5 V Fe–0.8 CH–1 [4]
U−B color index +0.09 [2]
B−V color index +0.61 [2]
Astrometry
Radial velocity (Rv)+2.1 [5]  km/s
Proper motion (μ)RA: +200.59 [1]   mas/yr
Dec.: +14.51 [1]   mas/yr
Parallax (π)49.50 ± 1.23  mas [1]
Distance 66 ± 2  ly
(20.2 ± 0.5  pc)
Absolute magnitude  (MV)4.05 [5] (4.94/4.87) [3]
Orbit [6]
Primary53 Aqr A
Companion53 Aqr B
Period (P)3500 yr
Semi-major axis (a)14.88″
Eccentricity (e)0.90
Inclination (i)44.13°
Longitude of the node (Ω)294.55°
Periastron epoch (T)B 2023
Argument of periastron (ω)
(secondary)		151.40°
Details
53 Aqr A
Mass 1.01 [7]   M☉
Radius 1.11 [8]   R☉
Luminosity 1.39 [8]   L☉
Surface gravity (log g)4.46 [3]   cgs
Temperature 5,922 [3]   K
Metallicity [Fe/H]–0.10 [3]   dex
Rotational velocity (v sin i)8 [9]  km/s
Age 0.18–0.37 [10]   Gyr
53 Aqr B
Mass 0.99 [7]   M☉
Surface gravity (log g)4.44 [3]   cgs
Temperature 5,811 [3]   K
Metallicity [Fe/H]–0.19 [3]   dex
Rotational velocity (v sin i)9 [9]  km/s
Other designations
GJ 859, HIP 110778. [11]
53 Aqr A: BD–17 6521, HD 212698, HR 8545, LTT 9026, SAO 165078.
53 Aqr B: BD–17 6520, HD 212697, HR 8544, LTT 9025, SAO 165077.
Database references
SIMBAD 53 Aqr
53 Aqr A
53 Aqr B

53 Aquarii (abbreviated 53 Aqr) is a binary star [12] system in the equatorial constellation of Aquarius. 53 Aquarii is its Flamsteed designation though the star also bears the Bayer designation of f Aquarii. The combined apparent visual magnitude of the pair is a 5.56, [2] making it just visible to the naked eye in dark suburban skies. Based upon an annual parallax shift of 49.50  milliarcseconds for the first component, this system is located at a distance of approximately 65 light-years (20 parsecs ) from Earth. [1]

This is a wide binary star system with a projected separation of 100  astronomical units; indicating that the two stars are at least this distance apart. [8] The primary component is a solar-type main sequence star with a stellar classification of G1 V. [4] It has about 99% of the Sun's mass, 111% of the Sun's radius, and shines with 139% of the luminosity of the Sun. [8] This energy is being emitted from an outer envelope at an effective temperature of 5,922 K, [3] giving it the golden hue of a G-type star. [13] An examination of the primary component with the Spitzer Space Telescope failed to detect any infrared excess that might otherwise be an indication of a circumstellar debris disk. [8]

The companion is a slightly cooler star with an effective temperature of 5,811 K. [3] It has a stellar classification of G5 V Fe–0.8 CH–1, [4] indicating it is a chemically peculiar G-type main sequence star showing an under-abundance of iron and the molecule CH in its spectrum. As of 2008, it has an angular separation of 1.325  arcseconds along a position angle of 30.9° from the primary. [14]

This system is coeval with the Castor Moving Group of stars that share a common motion through space; hence it is a candidate member of that association. This suggests that the system is young; its estimated age is in the range of 180 to 370 million years, based upon the spectrum and X-ray luminosity, respectively. [10]

Related Research Articles

<span class="mw-page-title-main">Delta Aquarii</span> Star in the constellation Aquarius

Delta Aquarii, officially named Skat, is the third-brightest star in the constellation of Aquarius. The apparent visual magnitude is 3.3, which can be seen with the naked eye. The distance to this star is about 113 light-years based upon parallax measurements, and it has a close companion.

<span class="mw-page-title-main">Beta Aquarii</span> Double star in the constellation Aquarius

Beta Aquarii is a single star in the constellation of Aquarius. It has the official name Sadalsuud and the Bayer designation β Aquarii, abbreviated Beta Aqr or β Aqr. Based upon parallax measurements obtained during the Hipparcos mission, this component is located at a distance of approximately 540 light years (165 parsecs) from the Sun. It is drifting further away with a radial velocity of 6.5 km/s. The star serves as an IAU radial velocity standard.

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

Xi Aquarii is a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of 4.7. Based upon parallax measurements made during the Hipparcos mission, this system lies at a distance of around 179 light-years from the Sun.

<span class="mw-page-title-main">Zeta Aquarii</span> Triple star system in constellation of Aquarius

Zeta Aquarii is the Bayer designation for a triple star system, the central star of the "water jar" asterism in the equatorial constellation of Aquarius. The combined apparent visual magnitude of this system is 3.65, which is readily visible to the naked eye. Parallax measurements yield a distance estimate of around 92 light-years from Earth.

<span class="mw-page-title-main">Phi Aquarii</span> Star in the constellation Aquarius

Phi Aquarii, Latinized from φ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with a combined apparent visual magnitude of +4.223. Parallax measurements indicate its distance from Earth is roughly 222 light-years, and it is drifting further away with a radial velocity of +2.5 km/s. It is 1.05 degrees south of the ecliptic so it is subject to lunar occultations.

<span class="mw-page-title-main">91 Aquarii</span> Triple star system in the constellation Aquarius

91 Aquarii is the Flamsteed designation for a triple star system in the equatorial constellation of Aquarius. It also bears the Bayer designation Psi1 Aquarii. It is visible to the naked eye with an apparent visual magnitude of +4.248. Parallax measurements yield an estimated distance of around 150 light-years from Earth. An extrasolar planet is known to orbit the main star.

Psi<sup>3</sup> Aquarii Binary star in the constellation Aquarius

Psi3 Aquarii, Latinized from ψ3 Aquarii, is the Bayer designation for a visual binary star system in the constellation of Aquarius. It has an apparent visual magnitude of 4.98, which is bright enough to be seen with the naked eye. Parallax measurements give a distance estimate of roughly 262 light-years.

<span class="mw-page-title-main">Mu Aquarii</span> Binary star system in the constellation Aquarius

Mu Aquarii, Latinized from μ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with a combined apparent visual magnitude of 4.7. Based upon parallax measurements, the distance to this system is about 157 light-years. It is drifting closer to the Sun with a radial velocity of −9.1 km/s.

<span class="mw-page-title-main">Upsilon Aquarii</span> Star in the constellation Aquarius

Upsilon Aquarii, Latinized from υ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.21. Parallax measurements give a distance estimate of 74.8 light-years from Earth. This is a high proper-motion star that is drifting closer to the Sun with a radial velocity of –2.3 km/s. It is part of the Hercules-Lyra association.

104 Aquarii (abbreviated 104 Aqr) is a star in the equatorial constellation of Aquarius. 104 Aquarii is the Flamsteed designation, although it also bears the Bayer designation A2 Aquarii. Based on an annual parallax shift of only 3.89 ± 0.25 milliarcseconds, the distance to this star is about 840 light-years (260 parsecs). At that range, the brightness of the star in the V-band is reduced by 0.10 magnitudes as a result of extinction caused by intervening gas and dust.

97 Aquarii is a binary star system in the equatorial constellation of Aquarius. 97 Aquarii is the Flamsteed designation. The combined apparent visual magnitude of the system is 5.20; the brighter star is magnitude 5.59 while the companion is magnitude 6.72. Based upon an annual parallax shift of 15.30 milliarcseconds, this system is at a distance of around 210 light-years from Earth.

94 Aquarii is a triple star system in the equatorial constellation of Aquarius. 94 Aquarii is the Flamsteed designation. The brightest member has an apparent visual magnitude of 5.19, making it visible to the naked eye. The parallax measured by the Gaia spacecraft yields a distance estimate of around 73 light-years from Earth.

107 Aquarii is a double star in the equatorial constellation of Aquarius. 107 Aquarii is the Flamsteed designation, although it also bears the Bayer designation i2 Aquarii. The pair have an angular separation of 6.787 arcseconds. They have a combined apparent visual magnitude of +5.305, with individual magnitudes of 5.72 and 6.72. The annual parallax shift measured for the two components is 16.1 mas and 20.0 mas respectively, although with significant statistical margins of error and flags for potential unreliability of both values. This indicates the system may be at a distance of 160–200 light-years from Earth.

96 Aquarii is a multiple star system in the zodiac constellation of Aquarius. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is faintly visible to the naked eye with an apparent visual magnitude of 5.56. The estimated distance to this system, based upon an annual parallax shift of 29.27 mas, is around 111 light years. The system has a relatively large proper motion and it is moving closer to the Sun with a radial velocity of −7 km/s.

51 Aquarii is a binary star system located around 410 light years away from the Sun in the equatorial constellation of Aquarius. 51 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.78. The system is moving further from the Earth with a heliocentric radial velocity of +6 km/s.

<span class="mw-page-title-main">74 Aquarii</span> Triple star system in the constellation Aquarius

74 Aquarii is a triple star system in the constellation of Aquarius. 74 Aquarii is its Flamsteed designation and it also bears the variable star designation HI Aquarii. The combined apparent visual magnitude is 5.8, although it is very slightly variable, and it is located at a distance of 590 light-years from Earth.

39 Aquarii is a star in the zodiac constellation of Aquarius. 39 Aquarii is its Flamsteed designation. It is a faint naked eye star with an apparent visual magnitude of 6.03. Based upon an annual parallax shift of 23.78 measured with a 3% margin of error, this star is at a distance of around 137 light-years from Earth. It is a double star with a magnitude 9.3 companion at an angular separation of 0.6 arcseconds along a position angle of 257°.

<span class="mw-page-title-main">29 Aquarii</span> Binary star in the constellation Aquarius

29 Aquarii is a binary star system located around 590 light years away from the Sun in the equatorial constellation of Aquarius. 29 Aquarii is the Flamsteed designation; the system also bears the variable star designation DX Aquarii. It is a challenge to view with the naked eye, appearing as a dim star with a combined apparent visual magnitude of 6.39. The system is moving further from the Earth with a heliocentric radial velocity of about +15 km/s.

<span class="mw-page-title-main">R Aquarii</span> Star in the constellation of Aquarius

R Aquarii is a variable star in the constellation Aquarius.

4 Aquarii is a binary star system in the constellation Aquarius, located approximately 198 light years away from the Sun. 4 Aquarii is the Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.99. The system is moving closer to the Earth with a heliocentric radial velocity of −21.5 km/s.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 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. 1 2 3 4 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
  3. 1 2 3 4 5 6 7 8 9 10 Pasquini, L.; Liu, Q.; Pallavicini, R. (July 1994), "Lithium abundances of nearby solar-like stars", Astronomy and Astrophysics, 287 (1): 191–205, Bibcode:1994A&A...287..191P.
  4. 1 2 3 Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I", The Astronomical Journal, 132 (1): 161–170, arXiv: astro-ph/0603770 , Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID   119476992.
  5. 1 2 Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv: astro-ph/0405198 , Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID   11027621.
  6. ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 1 August 2017. Retrieved 3 June 2017.
  7. 1 2 Cvetkovic, Z.; Ninkovic, S. (2010). "On the Component Masses of Visual Binaries". Serbian Astronomical Journal. 180 (180): 71–80. Bibcode:2010SerAJ.180...71C. doi: 10.2298/SAJ1080071C .
  8. 1 2 3 4 5 Plavchan, Peter; et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal, 698 (2): 1068–1094, arXiv: 0904.0819 , Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068, S2CID   51417657.
  9. 1 2 Torres, C. A. O.; et al. (December 2006), "Search for associations containing young stars (SACY). I. Sample and searching method", Astronomy and Astrophysics, 460 (3): 695–708, arXiv: astro-ph/0609258 , Bibcode:2006A&A...460..695T, doi:10.1051/0004-6361:20065602, S2CID   16080025.
  10. 1 2 Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv: 1007.1132 , Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948, S2CID   119209183.
  11. ↑ "53 Aqr". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2012-07-14. See also the children entries.
  12. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . S2CID   14878976.
  13. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
  14. ↑ Tokovinin, A.; Cantarutti, R. (February 2008), "First Speckle Interferometry at SOAR Telescope with Electron-Multiplication CCD", Publications of the Astronomical Society of the Pacific, 120 (864): 170–177, Bibcode:2008PASP..120..170T, doi: 10.1086/528809 .
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.