Iota Herculis

Iota Herculis

Historical view of the Hercules constellation showing Iota Herculis as one of the hero's feet.
Observation data
Epoch J2000      Equinox J2000
Constellation Hercules
Right ascension 17h 39m 27.8864s[1]
Declination +46° 00′ 22.795″[1]
Apparent magnitude (V) 3.7497[2]
Characteristics
Spectral type B3IV[1]
U−B color index –0.71
B−V color index –0.18[3]
Variable type Beta Cephei
Astrometry
Radial velocity (Rv)–20.0[1] km/s
Proper motion (μ) RA: 7.48[2] mas/yr
Dec.: 4.53[2] mas/yr
Parallax (π)7.17 ± 0.13[2] mas
Distance455 ± 8 ly
(139 ± 3 pc)
Absolute magnitude (MV)–1.97[4]
Details
Mass6.7 ± 0.1[5] M☉
Radius5.29 ± 0.45[6] R☉
Luminosity2,500[7] L☉
Surface gravity (log g)3.82 ± 0.06[6] cgs
Temperature18,070 ± 294[6] K
Metallicity [Fe/H]–0.40[8] dex
Rotational velocity (v sin i)11[9] km/s
Age37.8 ± 8.6[5] Myr
Other designations
ι Her, 85 Her, HR 6588, BD +46° 2349, HD 160762, FK5 663, HIP 86414, SAO 46872, GC 23965, CCDM J17395+4601A
Database references
SIMBADdata

Iota Herculis (ι Her, ι Herculis) is a fourth-magnitude variable star in the constellation Hercules.

Visibility

Small white disks representing the northern stars on a black background, overlaid by a circle showing the position of the north pole over time
The path of the north celestial pole among the stars due to the precession. Vega is the brightest star near the bottom, Iota Herculis is to the right near the -10000 hatch mark.

Iota Herculis is dim enough that in cities with a lot of light pollution it is unlikely to be visible with the naked eye. In rural areas it will usually be visible, and for much of the northern hemisphere the star is circumpolar and visible year around.

Pole Star

As a visible star, the proximity of Iota Herculis to the precessional path the Earth's North pole traces across the celestial sphere makes it a pole star, a title currently held by Polaris. In 10,000 BC it was the pole star, and in the future it will be again. While Polaris is only 0.5° off the precessional path Iota Herculis is 4° off.

Preceded by Pole Star Succeeded by
Vega ~16000 AD Tau Herculis

Properties

Iota Herculis is a B-type subgiant star that is at the end of its hydrogen fusion stage.[7] With a stellar classification B3IV, it is considerably larger than the Sun, having a mass that is 6.5 times solar and a radius 5.3 times. Though its apparent magnitude is only 3.79, it is 2,500 times more luminous than the Sun, yielding an absolute magnitude of -2.11, brighter in fact than the most of the hot B stars in the Pleiades open star cluster. The Hipparcos satellite mission estimated its distance at roughly 152 parsecs (pc) from Earth, or 496 light years (ly) away;[10] an updated parallax measurement from Floor van Leeuwen in 2007, however, puts the distance at 455ly with a much tighter error factor of only 8ly.[2]

Star system

Iota Herculis is a multiple star system. It is a spectroscopic binary having a 113.8 day period, indicating that its closest component is separated by about 1 AU.[7] Another companion can be found at approximately 30 AU from the main star, giving it an orbital period of about 60 years. Still another star has been identified with a common proper motion at an angular separation of 116 arcseconds and a visual magnitude of 12.1.[11] This would place it approximately 18,000 AU away, giving it an orbit of about 1 million years.[7]

Etymology

In Chinese, 天棓 (Tiān Bàng), meaning Celestial Flail, refers to an asterism consisting of ι Herculis, ξ Draconis, ν Draconis, β Draconis and γ Draconis.[12] Consequently, ι Herculis itself is known as 天棓五 (Tiān Bàng wu, English: the Fifth Star of Celestial Flail.)

References

  1. 1 2 3 4 "V* iot Her -- Variable Star of beta Cep type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-06-29.
  2. 1 2 3 4 5 van Leeuwen, F. (November 2007), "Hipparcos, the New Reduction", Astronomy and Astrophysics, Centre de Données astronomiques de Strasbourg, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, retrieved 2010-11-21
  3. ↑ Mermilliod, J.-C. (1986), Compilation of Eggen's UBV data, transformed to UBV (unpublished) (PDF)|format= requires |url= (help), Bibcode:1986EgUBV........0M, origin: SIMBAD
  4. ↑ Huang, W.; et al. (2012), "A catalogue of Paschen-line profiles in standard stars", Astronomy & Astrophysics, 547: A62, arXiv:1210.7893, Bibcode:2012A&A...547A..62H, doi:10.1051/0004-6361/201219804.
  5. 1 2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x
  6. 1 2 3 Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855
  7. 1 2 3 4 Kaler, James B., "IOTA HER (Iota Herculis)", Stars, University of Illinois, retrieved 2010-06-29
  8. ↑ Peters, Geraldine J.; Aller, Lawrence H. (1970), "The Chemical Composition of IOTA Herculis", The Astrophysical Journal (PDF)|format= requires |url= (help), 159: 525, Bibcode:1970ApJ...159..525P, doi:10.1086/150328
  9. ↑ "Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)", VizieR, Centre de Données astronomiques de Strasbourg, retrieved 2010-06-29
  10. ↑ Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; Hoeg, E.; et al. (1997). "The HIPPARCOS Catalogue". Astronomy and Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  11. ↑ "CCDM (Catalog of Components of Double & Multiple stars (Dommanget+ 2002)". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 2010-06-29.
  12. ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.

Coordinates: 17h 39m 27.8864s, +46° 00′ 22.795″

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