HD 37320

Last updated

HD 37320 (HR 1920, HIP 26487) is a star located in the constellation Orion. [lower-alpha 1] It is an evolved blue giant star, based on its spectral type of B8III. [1] The distance to HD 37320 is calculated at 285.5 parsecs (931 light-years), based on a parallax from Gaia EDR3. [2] The apparent magnitude of the star is 5.852, [1] which is above the limiting magnitude for naked-eye vision (6.5m), making it faintly visible to the naked eye. [3]

Contents

HD 37320
Observation data
Epoch J2000       Equinox J2000
Constellation Orion [lower-alpha 1]
Right ascension 05h 38m 01.12s [1]
Declination +07° 32′ 29.1″ [1]
Apparent magnitude  (V)5.852±0.009 [1]
Characteristics
Evolutionary stage Blue giant
Spectral type B7III [1]
Apparent magnitude  (U)5.44 [1]
Apparent magnitude  (B)5.788 [1]
Apparent magnitude  (G)5.844 [1]
Apparent magnitude  (J)5.933 [1]
Apparent magnitude  (H)5.997 [1]
Apparent magnitude  (K)5.964 [1]
Astrometry
Radial velocity (Rv)20.1±1 [4]  km/s
Proper motion (μ)RA: 10.602  mas/yr [4]
Dec.: -15.499  mas/yr [4]
Parallax (π)3.5025 ± 0.0568  mas [2]
Distance 930 ± 20  ly
(286 ± 5  pc)
Absolute magnitude  (MV)-1.43 [5]
Details
Mass 5.644±0.282 [6]   M☉
Radius 4.696 [lower-alpha 2]   R☉
Luminosity 218.78 [8]   L☉
Temperature 12,303 [8]   K
Rotational velocity (v sin i)25 [9]  km/s
Other designations
BD+07 953, Gaia DR2  3334369174165649536, Gaia DR3  3334369174165649536, HIP  26487, HR  1920, SAO  112979, PPM  149251, TIC  144611068, TYC  714-524-1, GSC  00714-00524, 2MASS J05380112+0732292
Database references
SIMBAD data

Characteristics

It is an evolved blue giant star with a spectral type of B8III. [1] It radiates about 219 times the solar luminosity by its photosphere at an effective temperature of 12,300 K. [8] Its uniform disk angular diameter is measured at 0.153  milliarcseconds. [7] At the estimated distance by Gaia EDR3, it yields a physical size of 4.696  R☉. The star has a mass of 5.644  M☉ [6] and rotates under its own axis at a speed of 25 km/s. [9]

HD 37320 is located within the constellation Orion, based on its astronomical coordinates. [lower-alpha 1] The distance to the star is 285.5 parsecs (931 light-years ), based on a parallax of 3.5025  mas from Gaia EDR3. [2] The apparent magnitude of the star, i.e. its brightness as seen from Earth, is of 5.852m, [1] which is above the limiting magnitude for naked-eye vision, generally defined as 6.5m, making it faintly visible to the naked eye. [3] The absolute magnitude of HD 37320, i.e. its brightness if it was seen at 10 parsecs (32.6 ly), is -1.43. [5] It is moving away from Earth at a velocity of 20.1 km/s. [4]

HD 37320 is the Henry Draper Catalogue designation for this star. Other designations include HR 1920 from the Bright Star Catalogue, HIP 26487 from the Hipparcos Catalogue and BD+07 953 from the Bonner Durchmusterung catalogue. [1]

Notes

  1. 1 2 3 Obtained with a right ascension of 05h 38m 01.12s and a declination of +07° 32′ 29.1″ [1] on this website.
  2. ↑ From an angular diameter of 0.153 milliarcseconds [7] and a distance of 285.5 parsecs. [2]

Related Research Articles

<span class="mw-page-title-main">Winnecke 4</span> Optical double star in the constellation Ursa Major

Winnecke 4 is an optical double star consisting of two unrelated stars in a northerly zone of the sky, Ursa Major.

N Centauri is a binary star in the southern constellation of Centaurus. The brighter star is dimly visible to the naked eye with an apparent visual magnitude of 5.26, and it is approximately 304 light years away based on parallax. It has an absolute magnitude of +0.76 and is drifting further away from the Sun with a radial velocity of +27 km/s. It is a candidate member of the Sco OB2 moving group.

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

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant.

<span class="mw-page-title-main">HD 155035</span> Star in the constellation Ara

HD 155035 is a star in the constellation Ara, the Altar. It is located at a distance of approximately 1,450 light-years from Earth and has an apparent visual magnitude of 5.92, making it is faintly visible to the naked eye. This is a red giant star with a stellar classification of M1.5 III. It an irregular variable that changes brightness over an amplitude range of 0.12 magnitudes.

HD 189276 is a single star in the northern constellation Cygnus, positioned near the northern constellation border with Draco. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.98. The star is located at a distance of approximately 820 light years from the Sun based on parallax, and it has an absolute magnitude of −2.25. It is drifting further away with a radial velocity of +4 km/s. The star has a high peculiar velocity of 38.5+1.8
−2.2 km/s and thus is a probable runaway star.

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

Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.

HD 83332 is a solitary, orange hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.68, making it faintly visible to the naked eye if viewed under ideal conditions. The star is located 285 light years away based on its annual parallax shift, but is drifting away with a radial velocity of 30 km/s.

HD 98176, also designated as HIP 55133 and rarely 22 G. Centauri, is a solitary, white hued star located in the southern constellation Centaurus. It has an apparent magnitude of 6.44, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 348 light years distant. At its current distance, its brightness is diminished by 0.32 magnitudes due to interstellar dust. Pauzen et al. (2001) lists it as a potential λ Boötis star.

HD 39901 is an orange hued star located in the constellation Columba. It is also called HR 2069, which is the star's Bright Star Catalog designation. Eggen (1989) lists it as a member of the old disk population.

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.

HD 49268 is a solitary star in the southern circumpolar constellation Volans. It has an apparent magnitude of +6.49, placing it near the limit of naked eye visibility. Parallax measurements place the object at a distance of 456 light years; it is receding with a heliocentric radial velocity of 20.6 km/s.

<span class="mw-page-title-main">Iota Mensae</span> Star in the constellation Mensa

Iota Mensae is a single star about 880 light years away in the faint constellation Mensa. It has a very slightly variable apparent magnitude of 6.0, making it visible with the naked eye under good skies.

HD 50002 is a solitary star in the southern circumpolar constellation Volans. It is faintly visible to the naked eye with an apparent magnitude of 6.09 and is located at a distance of 708 light years. However, it is drifting further with a heliocentric radial velocity of 5.1 km/s.

HD 155448 is a quintuple star system consisting of 5 young B-type stars. With an apparent magnitude of 8.72, it is too dim to be visible with the naked eye.

HD 191829 is a solitary star located in the southern constellation Telescopium. It has an apparent magnitude of 5.632, making it faintly visible to the naked eye if viewed under ideal conditions. The star is situated at a distance of 710 light years but is receding with a heliocentric radial velocity of 14 km/s.

HD 64307, also known as HR 3075, is a solitary, orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.35, allowing it to be faintly seen with the naked eye. Based on parallax measurements from the Gaia spacecraft, The object is estimated to be 690 light years distant. It appears to be receding from the Sun, having a heliocentric radial velocity of 34 km/s.

HD 33519, also known as HR 1682, is a probable spectroscopic binary located in the southern circumpolar constellation Mensa. It is one of the stars near the limit of naked eye visibility, having an apparent magnitude of 6.28. The system is relatively far at a distance of 940 light years but is approaching with a heliocentric radial velocity of −2.5 km/s. However, this value is poorly constrained.

74 Geminorum Giant star in the constellation Gemini

74 Geminorum is a K-type giant star in the constellation Gemini. It is located about 640 light-years from Earth based on its Gaia DR3 parallax. The star is often subject to lunar occultations, allowing an accurate measurement of its angular diameter. It has an apparent magnitude of 5.05, making it faintly visible to the naked eye.

HD 85945 is a star in the constellation Ursa Major. It is a yellow giant star with a spectral type of G6III:Fe-0.5. Based on information from Gaia DR3, it is located 132.54 parsecs (432.3 ly) from Earth and is moving towards Earth at a velocity of 47 km/s. It has an apparent magnitude of 5.96, which makes it faintly visible to the naked eye.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 "HD 37320". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2024-05-05.
  2. 1 2 3 4 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 .
  3. 1 2 "University Lowbrow Astronomers Naked Eye Observer's Guide". websites.umich.edu. Retrieved 2024-05-05.
  4. 1 2 3 4 Brandt, Timothy D. (2021-06-01). "The Hipparcos-Gaia Catalog of Accelerations: Gaia EDR3 Edition". The Astrophysical Journal Supplement Series. 254 (2): 42. arXiv: 2105.11662 . Bibcode:2021ApJS..254...42B. doi: 10.3847/1538-4365/abf93c . ISSN   0067-0049. Data about this star is available here at VizieR.
  5. 1 2 "HIP-26487 (Star)". In-the-sky. Retrieved 2024-05-05.
  6. 1 2 Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019-03-01). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy and Astrophysics. 623: A72. arXiv: 1811.08902 . Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. ISSN   0004-6361. Data about the star is available here at VizieR.
  7. 1 2 Challouf, M.; Nardetto, N.; Mourard, D.; Graczyk, D.; Aroui, H.; Chesneau, O.; Delaa, O.; Pietrzyński, G.; Gieren, W.; Ligi, R.; Meilland, A.; Perraut, K.; Tallon-Bosc, I.; McAlister, H.; Brummelaar, T. ten (2014-10-01). "Improving the surface brightness-color relation for early-type stars using optical interferometry". Astronomy & Astrophysics. 570: A104. arXiv: 1409.1351 . Bibcode:2014A&A...570A.104C. doi:10.1051/0004-6361/201423772. ISSN   0004-6361.
  8. 1 2 3 Simón-Díaz, S.; Godart, M.; Castro, N.; Herrero, A.; Aerts, C.; Puls, J.; Telting, J.; Grassitelli, L. (2017-01-01). "The IACOB project . III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars". Astronomy and Astrophysics. 597: A22. arXiv: 1608.05508 . Bibcode:2017A&A...597A..22S. doi:10.1051/0004-6361/201628541. ISSN   0004-6361. Data about the star is available here at VizieR.
  9. 1 2 Abt, Helmut A.; Levato, Hugo; Grosso, Monica (2002-07-01). "Rotational Velocities of B Stars". The Astrophysical Journal. 573 (1): 359–365. Bibcode:2002ApJ...573..359A. doi:10.1086/340590. ISSN   0004-637X. Available here in VizieR.
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.