49 Ceti

Last updated
49 Ceti
Cetus constellation map.svg
Red circle.svg
Location of 49 Ceti (circled)
Observation data
Epoch J2000        Equinox J2000
Constellation Cetus
Right ascension 01h 34m 37.77883s [1]
Declination −15° 40′ 34.8981″ [1]
Apparent magnitude  (V)5.607 [2]
Characteristics
Spectral type A1V [3]
U−B color index +0.05 [4]
B−V color index +0.07 [4]
Astrometry
Radial velocity (Rv)+10.30±0.7 [5]  km/s
Proper motion (μ)RA: 94.207 [1]   mas/yr
Dec.: -3.165 [1]   mas/yr
Parallax (π)17.5234 ± 0.1001  mas [1]
Distance 186 ± 1  ly
(57.1 ± 0.3  pc)
Details [6]
Mass 2.02  M☉
Luminosity 19.12  L☉
Surface gravity (log g)4.30 [7]   cgs
Temperature 8,790  K
Metallicity [Fe/H]0.10  dex
Rotational velocity (v sin i)196 km/s
Age 40 [8]   Myr
Other designations
BD−16°265, HD  9672, HIP  7345, HR  451, SAO  147886
Database references
SIMBAD data

49 Ceti is a single [9] star in the equatorial constellation of Cetus. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.607. [2] The star is located 186 light-years (57 parsecs) away from the Solar System, based on its parallax, [1] and is drifting further away with a radial velocity of +10 km/s. [5] 49 Ceti has been identified as a member of the 40-million-year-old Argus Association. [8]

This is a young A-type main-sequence star with a stellar classification of A1V. [3] It is about 40 [8]  million years old with a high rate of spin, showing a projected rotational velocity of 196 km/s. [6] The star has double the mass of the Sun. [6] It is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,790 K. [6]

49 Ceti displays a significant infrared excess, which is a characteristic of a debris disk orbiting the star. Unusually, the disk seems to be gas-rich, with evidence of carbon monoxide (CO) gas. This carbon monoxide gas may possibly be from comets orbiting the star within the disk, similar to the Kuiper Belt in the Solar System. [8]

Related Research Articles

<span class="mw-page-title-main">70 Virginis</span> Star in the constellation Virgo

70 Virginis is a binary star located 58 light years from the Sun in the equatorial constellation of Virgo, near the northern constellation border with Coma Berenices. 70 Virginis is its Flamsteed designation. The star is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of +4.97. It is drifting further away with a heliocentric radial velocity of +4.4 km/s and has a high proper motion, traversing the celestial sphere at the rate of 0.621 arc seconds per annum.

Mu Telescopii, Latinized from μ Telescopii is a solitary star in the southern constellation Telescopium. It has an apparent visual magnitude of 6.28, placing it near the limit of naked eye visibility. The object is relatively close at a distance of 118 light years but is receding with a heliocentric radial velocity of 8.6 km/s.

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

Sigma Andromedae, Latinized from σ Andromedae, is the Bayer designation for a single star in the northern constellation of Andromeda. It has an apparent visual magnitude of +4.5, which is bright enough to be seen with the naked eye from most locations. Parallax measurements made during the Gaia mission place it at a distance of about 140 light-years. The magnitude of the star is diminished by 0.08 from extinction caused by intervening gas and dust. It is drifting closer to the Sun with a radial velocity of –8 km/s.

Chi Boötis, Latinised as χ Boötis, is a single, white-hued star in the northern constellation Boötes, near the eastern constellation border with Corona Borealis. It is faintly visible to the naked eye with an apparent visual magnitude of +5.3. Based upon an annual parallax shift of 13.0 mas as seen from the Earth, it is located about 251 light-years from the Sun. The star is moving closer to the Sun with a radial velocity of −16 km/s.

Chi Cancri, Latinized from χ Cancri, is a candidate astrometric binary star system in the northern zodiac constellation of Cancer. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.14. The system is located at a distance of 59 light years from the Sun, based on parallax, and is drifting further away with a radial velocity of +33 km/s. It is estimated to have made its closest approach some 274,000 years ago when it came to within 42 light-years.

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

Alpha Chamaeleontis, Latinized from α Chamaeleontis, is a solitary star in the southern circumpolar constellation of Chamaeleon. It has an apparent visual magnitude of 4.06 and thus is bright enough to be seen with the naked eye. With an annual parallax shift of 51.12 mas, it is located 63.8 light years from the Sun. The star is drifting closer with a radial velocity of −13 km/s, and is predicted to come to within 47 light-years in 666,000 years.

94 Ceti is a trinary star system approximately 73 light-years away in the constellation Cetus.

24 Canum Venaticorum is a single star in the northern constellation of Canes Venatici, located 277 light years away from the Sun. This object is visible to the naked eye as a faint white-hued star with an apparent visual magnitude of +4.68. It is moving closer to the Earth with a heliocentric radial velocity of −18 km/s.

<span class="mw-page-title-main">HD 15115</span> F-type subgiant star in the constellation Cetus

HD 15115 is a single star in the equatorial constellation of Cetus. It is readily visible in binoculars or a small telescope, but is considered too dim to be seen with the naked eye at an apparent visual magnitude of 6.76. The distance to this object is 160 light years based on parallax, and it is slowly drifting further away at the rate of about 1 km/s. It has been proposed as a member of the Beta Pictoris moving group or the Tucana-Horologium association of co-moving stars; there is some ambiguity as to its true membership.

HD 88955 is a single, white-hued star in the southern constellation of Vela. It can be viewed with the naked eye, having an apparent visual magnitude of 3.85. The distance to HD 88955 can be determined from its annual parallax shift of 32.7 mas, which yields a separation of 100 light years from the Sun. It is moving further from the Earth with a heliocentric radial velocity of +7 km/s. Bayesian analysis suggests HD 88955 is a member of the Argus Association, a group of co-moving stars usually associated with the IC 2391 open cluster.

35 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39. An annual parallax shift of 16.9162±0.0681 mas provides a distance estimate of about 193 light years. It is moving closer with a heliocentric radial velocity of −8 km/s.

<span class="mw-page-title-main">5 Vulpeculae</span> Star in the constellation Vulpecula

5 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. It is situated amidst a random concentration of bright stars designated Collinder 399, or Brocchi's Cluster. This is a faint star that is just visible to the naked eye with an apparent visual magnitude of 5.60. Based upon an annual parallax shift of 13.8921±0.0900 mas, it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s, and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).

2 Ceti is a single star in the equatorial constellation of Cetus, near the border with Aquarius. It is visible to the naked eye with an apparent visual magnitude of 4.483. The distance to 2 Ceti can be estimated from its annual parallax shift of 12.0 mas, which yields a value of around 272 light years. It appears to be moving further from the Earth with a heliocentric radial velocity of about +8 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">HD 21278</span> Binary star system in the constellation Perseus

HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.

<span class="mw-page-title-main">29 Persei</span> Star in the constellation Perseus

29 Persei is a single star in the northern constellation of Perseus, located approximately 640 light years away from the Sun based on parallax. It is visible to the naked eye as faint, blue-white hued star with an apparent visual magnitude of 5.16. This object is a member of the Alpha Persei Cluster.

Phi Fornacis is a single star in the southern constellation of Fornax. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 5.13. The distance to this object is approximately 154 light-years based on parallax, and it is drifting further away with a radial velocity of +19 km/s.

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2 light years. It has a relatively high proper motion, advancing 262 mas per year across the celestial sphere.

HD 168009 is a star in the northern constellation of Lyra. It has an apparent visual magnitude of 6.3, placing it just above to below the normal limit of stars visible to the naked eye under good viewing conditions of 6-6.5. An annual parallax shift of 42.93 mas provides a distance estimate of 76 light years. It is moving closer to the Sun with a heliocentric radial velocity of −65 km/s. In about 328,000 years from now, the star will make its closest approach at a distance of around 17 ly (5.1 pc).

HD 46588 is a star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.44, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of only 59 light years but is receding with a heliocentric radial velocity of 15 km/s.

References

  1. 1 2 3 4 5 6 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 Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 Roberge, A.; Kamp, I.; Montesinos, B.; Dent, W. R. F.; Meeus, G.; Donaldson, J. K.; Olofsson, J.; Moór, A.; Augereau, J.-C.; Howard, C.; Eiroa, C.; Thi, W.-F.; Ardila, D. R.; Sandell, G.; Woitk e, P. (2013). "Herschel Observations of Gas and Dust in the Unusual 49 Ceti Debris Disk". The Astrophysical Journal. 771 (1): 69. arXiv: 1305.2894 . Bibcode:2013ApJ...771...69R. doi:10.1088/0004-637X/771/1/69. S2CID   1630036.
  4. 1 2 Rybka, E. (1969). "The corrected magnitudes and colours of 278 stars near S.A. 1-139 in the UBV system". Acta Astronomica. 19: 229. Bibcode:1969AcA....19..229R.
  5. 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.
  6. 1 2 3 4 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv: 1201.2052 . Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID   55586789.
  7. ↑ Pawellek, Nicole; et al. (September 2014), "Disk Radii and Grain Sizes in Herschel-resolved Debris Disks", The Astrophysical Journal, 792 (1): 19, arXiv: 1407.4579 , Bibcode:2014ApJ...792...65P, doi:10.1088/0004-637X/792/1/65, S2CID   119282523, 65.
  8. 1 2 3 4 Zuckerman, B.; Song, Inseok (2012). "A 40 Myr Old Gaseous Circumstellar Disk at 49 Ceti: Massive CO-Rich Comet Clouds at Young A-Type Stars". The Astrophysical Journal. 758 (2): 77. arXiv: 1207.1747 . Bibcode:2012ApJ...758...77Z. doi:10.1088/0004-637X/758/2/77. S2CID   119198485.
  9. ↑ 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.
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.