49 Orionis

Short description: Star in the constellation Orion

This page is about d Orionis. It is not to be confused with δ (delta) Orionis.

49 Orionis

Location of 49 Orionis (circled)

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Orion
Right ascension |  05h 38m 53.08332s[1]
Declination | −07° 12′ 46.1667″[1]
Apparent magnitude (V) | 4.80[2]
Characteristics
Evolutionary stage | main sequence
Spectral type | A4Vn[3]
U−B color index | +0.11[2]
B−V color index | +0.13[2]
Astrometry
Radial velocity (Rv)| −5.30[4] km/s
Proper motion (μ)|  RA: −15.562[1] mas/yr
Dec.: −50.613[1] mas/yr
Parallax (π)| 23.1346 ± 0.2801[1] mas
Distance| 141 ± 2 ly
(43.2 ± 0.5 pc)
Absolute magnitude (MV)| 1.52[5]
Details
Mass| 1.78[6] M☉
Radius| 2.0[7] R☉
Luminosity| 22[8] L☉
Surface gravity (log g)| 4.06[6] cgs
Temperature| 8,416±286[6] K
Rotational velocity (v sin i)| 186[8] km/s
Age| 284[6] Myr
Other designations

d Ori, 49 Ori, BD−07°1142, GC 7039, GJ 9187, HD 37507, HIP 26563, HR 1937, SAO 132411[9]

Database references
SIMBAD| data

49 Orionis is a single[10] star in the equatorial constellation of Orion. It has the Bayer designation d Orionis, while 49 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.80.[2] It is located 141 light years away from the Sun based on parallax,[1] but is drifting closer with a radial velocity of −5 km/s.[4]

49 Orionis (center)

In the past 49 Orionis was reported as a spectroscopic binary and an orbit was computed with a period of 445.74 days and an eccentricity of 0.549.[11] But it was later determined to be single.[10]

This object is an A-type main-sequence star with a stellar classification of A4Vn,[3] where the 'n' suffix indicates broadened "nebulous" lines caused by rapid rotation. It is around 284[6] million years old with a projected rotational velocity of 186 km/s.[8] This spin is giving the star an oblate shape with an equatorial bulge that is an estimated 8% larger than the polar radius.[12] The star has 1.8[6] times the mass of the Sun and double[7] the Sun's radius. It is radiating 22[8] times the Sun's luminosity from its photosphere at an effective temperature of 8,416 K.[6]

## References

1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
2. ↑ 2.0 2.1 2.2 2.3 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.
3. ↑ 3.0 3.1 Gray, R. O.; Garrison, R. F. (July 1989). "The Late A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation". Astrophysical Journal Supplement 70: 623. doi:10.1086/191349. Bibcode: 1989ApJS...70..623G.
4. ↑ 4.0 4.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
5. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. Vizier catalog entry
6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
7. ↑ 7.0 7.1 Allende Prieto, C.; Lambert, D. L. (1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures". Astronomy and Astrophysics 352: 555–562. Bibcode: 1999A&A...352..555A. Vizier catalog entry
8. ↑ 8.0 8.1 8.2 8.3 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. Bibcode: 2012A&A...537A.120Z. Vizier catalog entry
9. ↑ "49 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=49+Ori.
10. ↑ 10.0 10.1 De Rosa, R. J. et al. (2014). "The VAST Survey - III. The multiplicity of A-type stars within 75 pc". Monthly Notices of the Royal Astronomical Society 437 (2): 1216. doi:10.1093/mnras/stt1932. Bibcode: 2014MNRAS.437.1216D.
11. ↑ Abt, Helmut A. (June 1965). "The Frequency of Binaries among Normal A-Type Stars". Astrophysical Journal Supplement 11: 429. doi:10.1086/190120. Bibcode: 1965ApJS...11..429A.
12. ↑ Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review 20 (1): 51, doi:10.1007/s00159-012-0051-2, Bibcode: 2012A&ARv..20...51V.

* v
* t
* e

Stars of Orion

Bayer|

* α (Betelgeuse)
* β (Rigel)
* γ (Bellatrix)
* δ (Mintaka)
* ε (Alnilam)
* ζ (Alnitak)
* η (Algjebba)
* θ1
* Trapezium Cluster
* θ1 A
* θ1 B
* θ1 C
* θ1 D
* θ1 E
* θ2
* ι (Hatysa)
* κ (Saiph)
* λ (Meissa)
* μ
* ν
* ξ
* ο1
* ο2
* π1
* π2
* π3 (Tabit)
* π4
* π5
* π6
* ρ
* σ
* τ
* υ (Thabit)
* φ1
* φ2
* χ1
* χ2
* ψ1
* ψ2
* ω

Flamsteed|

* 5
* 6 (g)
* 11
* 13
* 14 (i)
* 15
* 16 (h)
* 18
* 21
* 22 (o)
* 23 (m)
* 27 (p)
* 29 (e)
* 31
* 32 (A)
* 33
* 35
* 38
* 42 (c)
* 45
* 49 (d)
* 51 (b)
* 52
* 55
* 56
* 57
* 59
* 60
* 63
* 64
* 66
* 68
* 69 (f1)
* 71
* 72 (f2)
* 73
* 74 (k)
* 75 (l)

Variable|

* S
* T
* U
* W
* Z
* RS
* UX
* VV
* VY
* YY
* AN
* BF
* BL
* BM
* BN
* BQ
* CK
* CN
* CO
* CZ
* DN
* DY
* ER
* EW
* EY
* FH
* FT
* FU
* FZ
* GG
* GP
* GU
* GW
* HK
* KX
* V346
* V351
* V359
* V371
* V372
* V380
* V586
* V883
* V901
* V1031
* V1046
* V1051
* V1107
* V1118
* V1149
* V1155
* V1156
* V1159
* V1162
* V1179
* V1192
* V1197
* V1261
* V1307
* V1309
* V1355
* V1357
* V1366
* V1369
* V1377
* V1389
* V1647
* V1649
* V1788

HR|

* 1507
* 1519
* 1522
* 1534
* 1553
* 1571
* 1574
* 1576
* 1578
* 1591
* 1596
* 1600
* 1613
* 1618
* 1619
* 1646
* 1681
* 1684
* 1685
* 1687
* 1691
* 1697
* 1701
* 1703
* 1709
* 1717
* 1724
* 1748
* 1759
* 1763
* 1764
* 1778
* 1781
* 1782
* 1786
* 1799
* 1803
* 1806
* 1807
* 1809
* 1819
* 1820
* 1826
* 1830
* 1832
* 1833
* 1840
* 1848
* 1861
* 1873
* 1874
* 1883
* 1886
* 1887
* 1891
* 1908
* 1911
* 1913
* 1918
* 1920
* 1923
* 1933
* 1940
* 1942
* 1950
* 1952
* 1955
* 1959
* 1967
* 1978
* 1986
* 1987
* 1988
* 2007
* 2014
* 2019
* 2024
* 2030
* 2039
* 2048
* 2051
* 2057
* 2070
* 2071
* 2075
* 2076
* 2093
* 2097
* 2099
* 2113
* 2133
* 2174
* 2184
* 2191
* 2214
* 2218
* 2222
* 2231
* 2233
* 2235
* 2236
* 2251
* 2253
* 2259
* 2269
* 2275
* 2287
* 2302

HD|

* 30869
* 31253
* 31423
* 33636
* 34445
* 35575
* 35775
* 36150
* 36558
* 36629
* 36814
* 36840
* 37605
* 37806
* 37903
* 38087
* 38801
* 290327

Gliese|

* Gliese 179
* Gliese 182
* Gliese 205
* Gliese 208
* Gliese 221
* GJ 3379

Other|

* BD +03 740
* Becklin–Neugebauer Object
* CVSO 30
* G 99-37
* G 99-47
* LkHα 208
* LP 658-2
* 2MASS J05352184-0546085
* OMC-2 FIR 4
* Orion source I
* Reipurth 50
* Ross 47
* RX J0529.4+0041
* S Ori 52
* S Ori 70
* 4U 0614+091
* WISE J0457−0207
* WISE J0521+1025

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