HR 3600

Last updated

HR 3600
Vela constellation map.svg
Red circle.svg
Location of HR 3600 (circled)
Observation data
Epoch J2000 [1]        Equinox J2000 [1]
Constellation Vela
Right ascension 09h 01m 20.86511s
Declination −41° 51′ 51.3343″
Apparent magnitude  (V)+5.541 [2]
Characteristics
HR 3562A
Spectral type B5V [3]
U−B color index −0.56 [2] [4]
B−V color index −0.133 [2]
J−H color index −0.106 [4]
J−K color index −0.106 [4]
Variable type Slowly pulsating B-type star? [5]
Astrometry
Radial velocity (Rv)22.8±1.2 [6]  km/s
Proper motion (μ)RA: -22.727 [7]   mas/yr
Dec.: 12.139 [7]   mas/yr
Parallax (π)6.6050 ± 0.0711  mas [7]
Distance 494 ± 5  ly
(151 ± 2  pc)
Absolute magnitude  (MV)−0.71 [8]
Absolute bolometric
magnitude  (Mbol)		−2.08 [8]
Details [8]
Mass 3.999±0.200 [9]   M☉
Radius 3.222±0.161 [9]   R☉
Luminosity 535  L☉
Surface gravity (log g)4.30  cgs
Temperature 14,966  K
Rotational velocity (v sin i)50 [5]  km/s
Other designations
IZ Velorum, CD−41° 4720, CPD−41° 3232, Gaia DR3  5428323854487771392, GC  12489, HD  77475, HIP  44299, HR  3600, SAO  220760, PPM  313879, WDS J08553-4503A, TIC  191446158, TYC  7685-2721-1, GSC  07685-02721, 2MASS J09012085-4151513 [1]
Database references
SIMBAD data

HR 3600 (HD 77475) is a bluish-white hued variable star in the southern constellation of Vela. It has the variable-star designation IZ Velorum (abbreviated to IZ Vel). With an apparent magnitude of about 5.54, it is faintly visible by the naked eye under dark skies. It is located approximately 494 light-years (151 parsecs) distant according to Gaia EDR3 parallax measurements, and is receding from the Solar System at a heliocentric radial velocity of 22.8 km/s.

Physical properties

This is a hot, luminous B-type main-sequence star with a mass of 4.0 M☉ and a radius of 3.2 R☉. [9] With an effective temperature of 14,966 K (26,479 °F), it shines at an absolute bolometric magnitude of −2.08, meaning it radiates 535 L☉ from its photosphere; and an absolute visual magnitude of −0.71, that is 151 L☉ released in the visual (V) band of the UBV photometric system. [8]

This star was initially given the stellar classification B5III in 1978, [10] indicative of a blue giant, but was reclassified as a main-sequence star of the same spectral type by Burki et al. (1982) due to similarities to other stars such as 32 Orionis, Lambda Columbae, HW Velorum, and HD 186837, all of type B5V. They simultaneously reported that it was a slowly pulsating B-type star (SPB) with three tentative periods of 9.64 days, 14.4 days, and 10.7 days, all of them with amplitudes of several mmag that produce a combined peak-to-peak amplitude of roughly 0.03 mag. [3]

A light curve for IZ Velorum, plotted from TESS data. The 0.905 day period derived by Balona is marked in red. IZVelLightCurve.png
A light curve for IZ Velorum, plotted from TESS data. The 0.905 day period derived by Balona is marked in red.

In 1986, Balona & Laing stated that HR 3600 in fact only had a single period of 1.10 days, an alias of the 9.64-day period presented by Burki et al. Citing the variable radial velocity of the star (20-30 km/s) and the low projected rotational velocity (50 km/s), they argued that it was more likely a rotating ellipsoidal variable, in which case the system would consist of a close binary orbiting each other every 2.20 days. [12] In 1994, Balona, who continued to observe the variable, revised the period to 0.905 days (or possibly 1.81 days), which was another alias of the 9.64-day period. The 14.4-day period could not be detected. The low rotational velocity contradicts with the hypotheses that the variability is caused by either binarity or rotational modulation, so the exact nature of this star has yet to be determined. [5]

Related Research Articles

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

Phi Velorum is a star in the constellation Vela. It is a blue-white B-type supergiant with an apparent magnitude of +3.53. It is approximately 1,590 light years from Earth.

<span class="mw-page-title-main">Iota Boötis</span> Binary star system in the northern constellation of Boötes

Iota Boötis is a member of a binary star system in the constellation Boötes, approximately 96 light-years from Earth. It has the traditional name Asellus Secundus and the Flamsteed designation 21 Boötis. The companion is HD 234121, a K0 main sequence star.

<span class="mw-page-title-main">Kappa Boötis</span> Double star in the constellation of Boötes

Kappa Boötis is a double star in the constellation Boötes. It has the traditional name Asellus Tertius and the Flamsteed designation 17 Boötis. The components are separated by an angular distance of 13.5 arcsec, viewable in a small telescope. Kappa Boötis is approximately 155 light years from Earth.

<span class="mw-page-title-main">10 Canis Majoris</span> Star in the constellation Canis Major

10 Canis Majoris is a single variable star in the southern constellation of Canis Major, located roughly 1,980 light years away from the Sun. It has the variable star designation FT Canis Majoris; 10 Canis Majoris is the Flamsteed designation. This body is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.23. It is moving away from the Earth with a heliocentric radial velocity of +34 km/s.

<span class="mw-page-title-main">HD 74180</span> Supergiant star in the constellation Vela

HD 74180 is a single star in the constellation Vela. It is a yellow-white F-type supergiant with a mean apparent magnitude of +3.81 and a spectral classification F8Ib. Estimates of its distance to Earth vary between 3,200 and 8,300 light-years.

<span class="mw-page-title-main">HD 183144</span> Suspected variable star in the constellation Aquila

HD 183144 is a suspected variable star in the equatorial constellation of Aquila. It is a hot giant star about 1,130 light years away.

<span class="mw-page-title-main">89 Herculis</span> Star in the constellation Hercules

89 Herculis is a binary star system located about 4,700 light years away from the Sun in the northern constellation of Hercules. It is visible to the naked eye as a faint, fifth magnitude star. The system is moving closer to the Earth with a heliocentric radial velocity of −28.5 km/s.

<span class="mw-page-title-main">V381 Cephei</span> Triple star system in the constellation Cepheus

V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

<span class="mw-page-title-main">WR 22</span> Binary star in the constellation Carina

WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright X-ray source due to colliding winds with a less massive O class companion. Its eclipsing nature and apparent magnitude make it very useful for constraining the properties of luminous hydrogen-rich WR stars.

<span class="mw-page-title-main">HD 168607</span> Star in the constellation Sagittarius

HD 168607 is a blue hypergiant and luminous blue variable (LBV) star located in the constellation of Sagittarius, easy to see with amateur telescopes. It forms a pair with HD 168625, also a blue hypergiant and possible luminous blue variable, that can be seen at the south-east of M17, the Omega Nebula.

<span class="mw-page-title-main">W Crucis</span> Variable star in the constellation Crux

W Crucis is a single-lined eclipsing variable star system in the constellation Crux. It has a spectral class of F8/G1Ia/abe indicating a yellow supergiant with emission lines in its spectrum.

HD 122862 is a solitary star in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.02, allowing it to be faintly seen with the naked eye under ideal conditions. The star is relatively close at a distance of 95 light years, but is approaching the Sun with a radial velocity of −21.11 km/s.

<span class="mw-page-title-main">V915 Scorpii</span> Variable star in the constellation Scorpius

V915 Scorpii is a hypergiant and semiregular variable star, located 1,718 parsecs (5,600 ly) away in the constellation Scorpius. Its apparent magnitude varies between 6.22 and 6.64, being heavily diminshed by 2.93 magnitudes due to interstellar extinction. When it is at its brightest, it is very faintly visible to the naked eye under excellent observing conditions.

HD 76270, also known as HR 3544, is a solitary, white hued star located in the southern circumpolar constellation Volans. It has an apparent magnitude of 6.10, making it faintly visible to the naked eye if viewed under ideal conditions. The object is relatively far with a distance of 2,360 light years, but is slowly approaching the Solar System with a heliocentric radial velocity of −2.6 km/s.

<span class="mw-page-title-main">HD 152408</span> Star in the constellation of Scorpius

HD 152408, also known as WR 79a, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 2,020 parsecs away from the Earth.

<span class="mw-page-title-main">HD 326823</span> Binary star system in the constellation of Scorpius

HD 326823, also known as V1104 Scorpii, is a binary star containing a unique emission-line star, which is in the midst of transitioning to a nitrogen-rich Wolf-Rayet star, as well as being a candidate Luminous blue variable, located 4,142 light years away in the constellation of Scorpius. The primary is very evolved, because it is composed of almost entirely helium, and only 3% of it is still hydrogen, and it has lost most of its mass to the now-very-massive secondary. The underlying mechanisms and mass transfers in the system are comparable to other W Serpentis systems, such as Beta Lyrae and RY Scuti.

HD 194612 is a solitary orange hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.9, making it visible to the naked eye under ideal conditions. Parallax measurements place it at a distance of 760 light years and it has a low heliocentric radial velocity of 0.3 km/s.

<span class="mw-page-title-main">HR 1217</span> Star in the constellation Eridanus

HR 1217 is a variable star in the constellation Eridanus. It has the variable star designation DO Eridani, but this seldom appears in the astronomical literature; it is usually called either HR 1217 or HD 24712. At its brightest, HR 1217 has an apparent magnitude of 5.97, making it very faintly visible to the naked eye for an observer with excellent dark-sky conditions.

<span class="mw-page-title-main">HD 123</span> Triple star system in the constellation Cassiopeia

HD 123 is a hierarchical triple star system in the deep northern constellation of Cassiopeia. It consists of a visual binary between HD 123A and B, of which component B is itself a spectroscopic binary. Through the use of a telescope, the visual pair can be resolved, with a separation that varies between 0.5 and 1.6 arcseconds. With a combined apparent magnitude of 5.98, it is faintly visible to the naked eye under dark skies as a yellow-hued star. The system is located approximately 70 light-years (21 pc) distant according to Hipparcos parallax measurements, while the Gaia EDR3 parallaxes for the individual stars point towards slightly closer distances of 67.8 ly (20.8 pc) and 69.4 ly (21.3 pc), respectively. It is trending closer towards the Solar System at a heliocentric radial velocity of −13.79 km/s.

<span class="mw-page-title-main">HR 3562</span> Visual binary in constellation Vela

HR 3562 is a visual binary consisting of a bluish-white hued variable star and a Sun-like secondary star in the southern constellation of Vela. It has the variable-star designation IY Velorum. With an apparent magnitude of 6.26, the brighter primary is near the limit for naked eye visibility. The fainter companion has an apparent magnitude of 12.639 and can be observed with a telescope with an aperture of 76 mm or wider. It is located approximately 373 parsecs (1,220 ly) distant according to Gaia EDR3 parallax measurements, and is receding away from the Solar System at a heliocentric radial velocity of 22.0 km/s.

References

  1. 1 2 3 "HD 77475". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 11 January 2025.
  2. 1 2 3 Høg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics. 355 (1): L27 –L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 Burki, G.; Burnet, M.; Magalhaes, A. S.; North, P.; Rufener, F.; Waelkens, C. (19 October 1982). "HR 3562 and HR 3600, Two New Multi-Periodic B-Type Stars". Information Bulletin on Variable Stars. 2211 (1). Konkoly Observatory, Budapest: International Astronomical Union. Bibcode:1982IBVS.2211....1B.
  4. 1 2 3 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  5. 1 2 3 Balona, L. A. (15 October 1994). "The 53 Per stars HR 3562 and HR 3600" (PDF). Monthly Notices of the Royal Astronomical Society. 270 (4): 914–920. doi: 10.1093/mnras/270.4.914 . ISSN   0035-8711 . Retrieved 7 January 2025.
  6. ↑ 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 . doi: 10.1134/S1063773706110065 . ISSN   1063-7737 . Retrieved 9 January 2025.
  7. 1 2 3 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.
  8. 1 2 3 4 North, P.; Paltani, S. (August 1994). "HD 37151: a new "slowly pulsating B star"". Astronomy & Astrophysics. 288: 155–164. Bibcode:1994A&A...288..155N.
  9. 1 2 3 Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019). "Stellar and substellar companions of nearby stars from Gaia DR2: Binarity from proper motion anomaly" (PDF). Astronomy & Astrophysics. 623: A72. doi: 10.1051/0004-6361/201834371 . ISSN   0004-6361 . Retrieved 7 January 2025. Record for this source at VizieR.
  10. ↑ Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  11. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 10 January 2025.
  12. ↑ Balona, L. A.; Laing, J. D. (1 December 1986). "HR 3562 and 3600: two short-period B-type variables". Monthly Notices of the Royal Astronomical Society. 223 (3): 621–627. doi: 10.1093/mnras/223.3.621 . ISSN   0035-8711.
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.