Astronomy:HD 161056

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Short description: Star in the constellation Ophiuchus
HD 161056
Location of HD 161056 (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ophiuchus[1]
Right ascension  17h 43m 47.02216s[2]
Declination −07° 04′ 46.5943″[2]
Apparent magnitude (V) 6.32[3]
Characteristics
Spectral type B1.5V, B3II/III, or B3Vn[4]
U−B color index −0.42[3]
B−V color index 0.36[3]
J−H color index 0.072[5]
J−K color index 0.101[5]
Astrometry
Radial velocity (Rv)−26.0±4.3[6] km/s
Proper motion (μ) RA: −4.629[2] mas/yr
Dec.: −10.512[2] mas/yr
Parallax (π)2.4404 ± 0.0432[2] mas
Distance1,340 ± 20 ly
(410 ± 7 pc)
Absolute magnitude (MV)−1.23[1]
Details
Mass12.5[7] M☉
Radius11.7[2] R☉
Luminosity14,454[7] L☉
Surface gravity (log g)3.26[2] cgs
Temperature26,977[7] K
Metallicity [Fe/H]−0.01[8] dex
Rotational velocity (v sin i)234[9] km/s
Age522[8] Myr
Other designations
BD−07°4487, GC 24051, HIP 86768, HR 6601, SAO 141832, PPM 200979, TYC 5093-438-1, 2MASS J17434702-0704465[5]
Database references
SIMBADdata

HD 161056 (HIP 86768, HR 6601) is a bluish-white hued star in the equatorial constellation of Ophiuchus. It has an apparent magnitude of 6.32, placing it near the limit for naked eye visibility under dark skies. The object is located approximately 1,340 light-years (410 parsecs) distant according to Gaia DR3 parallax measurements,[2] but it is moving closer at a heliocentric radial velocity of −26.0 km/s.

It is a luminous early B-type star, but its spectral type varies from publication to publication, most often between B1.5V,[10] implying a hot main-sequence star, and B3II/III,[11] indicative of a slightly cooler blue giant. It has a mass of 12.5 M☉ and a radius of 11.7 R☉.

In Chinese astronomy, the star was given the name Shìlóuliù (Chinese: 市樓六), meaning it was the sixth star of the asterism Shìlóu (市樓, "Municipal Office") in the Heavenly Market enclosure.[12]

Polarimetry

In 1985, the star was suggested as a standard for polarimetric observations via the Hubble Space Telescope, since the star's large distance from Earth produces a large interstellar polarization and its high luminosity makes it easily visible at such distances. In 1988, however, it was found that the star was slightly variable in polarization,[lower-alpha 1] and thus unsuitable as a standard star.[13]

Nevertheless, Hubble observed the star's ultraviolet interstellar polarization, thanks to it having been well-researched in the visible spectrum, presenting results consistent with Serkowski's law[14]—an empirical formula regarding the dependency of interstellar polarization on wavelength.[15] The extensive collected polarization spectrum showed a close match to what would be expected from an interstellar dust composition of pure amorphous forsterite.[16]

Spectroscopy

In addition to polarimetry, spectroscopic observations have also been conducted on HD 161056 to provide insight into the interstellar medium. The ESO Diffuse Interstellar Bands Large Exploration Survey (EDIBLES) detected signatures of diatomic carbon and tricarbon molecules in interstellar clouds surrounding the star.[17]

Near-infrared spectroscopy has revealed signs of weak stellar emission lines of singly ionized magnesium and neutral helium (Mg II and He I in spectroscopic notation).[18]

Runaway star

HD 161056 is a runaway star and a candidate for producing a bow shock observable in the infrared.[19] Such stars commonly originate in multiple star systems, from which they were ejected due to gravitational interactions or supernovae of their companions,[20] and indeed it is possible that the star could have been in a binary system with the pulsar PSR B1929+10 about 1.1 million years ago, when it was located in the vicinity of IC 4665. However, Zeta Ophiuchi is considered more likely to have been its binary companion, in which scenario the pair possibly split up around 900,000 years ago.[21]

See also

Notes

  1. ↑ The same authors backed the star's status down to "possibly variable" in a 2007 study.[10]

References

  1. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 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. 
  4. ↑ Pantaleoni González, M; Maíz Apellániz, J; Barbá, R H; Reed, B Cameron (2021-03-19). "The Alma catalogue of OB stars – II. A cross-match with Gaia DR2 and an updated map of the solar neighbourhood". Monthly Notices of the Royal Astronomical Society (Oxford University Press (OUP)) 504 (2): 2968–2982. doi:10.1093/mnras/stab688. ISSN 0035-8711.  Record for this source at VizieR.
  5. ↑ 5.0 5.1 5.2 "HD 161056". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+161056. 
  6. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters (Pleiades Publishing Ltd) 32 (11): 759–771. doi:10.1134/s1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 7.2 Quintana, Alexis L.; Wright, Nicholas J.; Martínez García, Juan (2025). "A census of OB stars within 1 KPC and the star formation and core collapse supernova rates of the Milky Way". Monthly Notices of the Royal Astronomical Society 538 (3): 1367. doi:10.1093/mnras/staf083. Bibcode: 2025MNRAS.538.1367Q. 
  8. ↑ 8.0 8.1 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters 38 (12): 771–782. doi:10.1134/S1063773712120031. ISSN 1063-7737. Bibcode: 2012AstL...38..771G. 
  9. ↑ Strom, Stephen E. et al. (February 2005). "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?". The Astronomical Journal 129 (2): 809–828. doi:10.1086/426748. Bibcode: 2005AJ....129..809S. 
  10. ↑ 10.0 10.1 Bastien, P.; Vernet, E.; Drissen, L.; Menard, F.; Moffat, A. F. J.; Robert, C.; St-Louis, N. (April 2007). "The variability of polarized standard stars". in Sterken, C.. The Future of Photometric, Spectrophotometric and Polarimetric Standardization. 364. Astronomical Society of the Pacific. p. 529. Bibcode: 2007ASPC..364..529B. 
  11. ↑ Wiktorowicz, Sloane J.; Słowikowska, Agnieszka; Nofi, Larissa A.; Rider, Nicole; Wolfgang, Angie; Hermis, Ninos; Jontof-Hutter, Daniel; Bayless, Amanda J. et al. (2023-02-01). "A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter". The Astrophysical Journal Supplement Series (American Astronomical Society) 264 (2): 42. doi:10.3847/1538-4365/aca407. ISSN 0067-0049. Bibcode: 2023ApJS..264...42W. 
  12. ↑ Yi, Shitong (April 1981). 科学出版社. 
  13. ↑ Bastien, P.; Drissen, L.; Menard, F.; Moffat, A. F. J.; Robert, C.; St-Louis, N. (1988). "The variability of polarized standard stars". The Astronomical Journal (American Astronomical Society) 95: 900. doi:10.1086/114688. ISSN 0004-6256. Bibcode: 1988AJ.....95..900B. 
  14. ↑ Somerville, W. B.; Allen, R. G.; Carnochan, D. J.; He, Lida; McNally, D.; Martin, P. G.; Morgan, D. H.; Nandy, K. et al. (1994). "Ultraviolet interstellar polarization observed with the Hubble Space Telescope". The Astrophysical Journal (American Astronomical Society) 427: L47. doi:10.1086/187361. ISSN 0004-637X. Bibcode: 1994ApJ...427L..47S. 
  15. ↑ Mathis, John S. (1990). "Interstellar Dust and Extinction". Annual Review of Astronomy and Astrophysics (Annual Reviews) 28 (1): 37–70. doi:10.1146/annurev.aa.28.090190.000345. ISSN 0066-4146. Bibcode: 1990ARA&A..28...37M. https://ned.ipac.caltech.edu/level5/Mathis/Mathis5_1.html. 
  16. ↑ Papoular, Renaud (2018-06-12). "A new interpretation of Serkowski's polarization law". Monthly Notices of the Royal Astronomical Society (Oxford University Press (OUP)) 479 (2): 1685–1693. doi:10.1093/mnras/sty1530. ISSN 0035-8711. 
  17. ↑ Fan, Haoyu; Rocha, Carlos M. R.; Cordiner, Martin; Linnartz, Harold; Cox, Nick L. J.; Farhang, Amin; Smoker, Jonathan; Roueff, Evelyne et al. (2023-12-22). "The EDIBLES survey". Astronomy & Astrophysics (EDP Sciences) 681: A6. doi:10.1051/0004-6361/202243910. ISSN 0004-6361. 
  18. ↑ Cox, N. L. J.; Cami, J.; Kaper, L.; Ehrenfreund, P.; Foing, B. H.; Ochsendorf, B. B.; van Hooff, S. H. M.; Salama, F. (2014). "VLT/X-Shooter survey of near-infrared diffuse interstellar bands". Astronomy & Astrophysics (EDP Sciences) 569: A117. doi:10.1051/0004-6361/201323061. ISSN 0004-6361. Bibcode: 2014A&A...569A.117C. 
  19. ↑ Peri, C. S.; Benaglia, P.; Isequilla, N. L. (2015). "E-BOSS: An Extensive stellar BOw Shock Survey". Astronomy & Astrophysics (EDP Sciences) 578: A45. doi:10.1051/0004-6361/201424676. ISSN 0004-6361. 
  20. ↑ Hoogerwerf, R.; de Bruijne, J. H. J.; de Zeeuw, P. T. (2000-12-01). "The Origin of Runaway Stars". The Astrophysical Journal (American Astronomical Society) 544 (2): L133–L136. doi:10.1086/317315. ISSN 0004-637X. Bibcode: 2000ApJ...544L.133H. 
  21. ↑ Bobylev, V. V. (2008-09-29). "Open clusters IC 4665 and Cr 359 and a probable birthplace of the pulsar PSR B1929+10". Astronomy Letters (Pleiades Publishing Ltd) 34 (10): 686–698. doi:10.1134/s1063773708100046. ISSN 1063-7737. Bibcode: 2008AstL...34..686B. 



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