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Iota1 Normae

From Wikipedia, the free encyclopedia
Star in the constellation Norma
For other star systems with thisBayer designation, seeι Normae.
ι1 Normae
Location of ι1 Normae (circled in red)
Observation data
Epoch J2000      Equinox J2000
ConstellationNorma
ι1 Nor AB
Right ascension16h 03m 32.08942s[1]
Declination−57° 46′ 30.2641″[1]
Apparent magnitude (V)5.14 + 5.70[2]
ι1 Nor C
Right ascension16h 03m 30.86534s[3]
Declination−57° 46′ 35.2404″[3]
Apparent magnitude (V)8.02 (8.75 + 8.75)[2]
Characteristics
ι1 Nor AB
Spectral typeA4 V + A6 V[4]
ι1 Nor C
Spectral typeG8V + K4V[5]
Variable typesuspectedRS CVn[5]
Astrometry
ι1 Nor AB
Radial velocity (Rv)−14.4±3.7[6] km/s
Proper motion (μ)RA: −120.01[1]mas/yr
Dec.: −82.09[1]mas/yr
Parallax (π)24.67 mas[7]
Distance132.2 ly
(40.54 pc)[7]
ι1 Nor C
Radial velocity (Rv)−10.0±0.7[7] km/s
Proper motion (μ)RA: −117.271mas/yr[3]
Dec.: −85.238mas/yr[3]
Parallax (π)24.3136±0.0220 mas[3]
Distance134.1 ± 0.1 ly
(41.13 ± 0.04 pc)
Orbit[8]
Primaryι1 Nor A
Companionι1 Nor B
Period (P)26.84±0.09 yr
Semi-major axis (a)0.328±0.006
Eccentricity (e)0.515±0.012
Inclination (i)168.7±9.9°
Longitude of the node (Ω)42.0±43.2°
Periastronepoch (T)1990.87±0.21
Argument of periastron (ω)
(secondary)
320.0±44.1°
Orbit[7]
Primaryι1 Nor Ca
Companionι1 Nor Cb
Period (P)0.82346(1) days
Semi-major axis (a)0.512 mas[2]
Eccentricity (e)0(assumed)
Inclination (i)~45°
Argument of periastron (ω)
(secondary)
0(assumed)°
Semi-amplitude (K1)
(primary)
107.0±1.2 km/s
Semi-amplitude (K2)
(secondary)
124.7±2.1 km/s
Details
ι1 Nor A
Mass1.75[2] M
ι1 Nor B
Mass1.54[2] M
ι1 Nor Ca
Mass0.88[2] M
ι1 Nor Cb
Mass0.88[2] M
Other designations
ι1 Nor,CPD−57°7500,HR 5961,WDS J16035-5747[9]
AB:HD 143474,HIP 78662,SAO 243279
C:SAO 243278
Database references
SIMBADdata
C

Iota1 Normae (ι1 Normae) is aquadruple star system[7] in the southernconstellation ofNorma. With a combinedapparent visual magnitude of 4.63,[2] it is faintly visible to the naked eye.Stellar parallax measurements give distances varying between 132.2 and 134.1 light-years. At that distance, the visual magnitude of these stars is diminished by anextinction of 0.062 magnitudes due tointerstellar dust.[10]

The inner pair orbit each other with aperiod of 26.8 years, asemimajor axis of 0.33 arc seconds, and aneccentricity of 0.515. Both stars areA-type main sequence stars. The brighter of the pair, magnitude 5.14[2] component A, has a spectral class of A4 V,[4] while its magnitude 5.70[2] companion, component B, is of class A6 V.[4] The two are 1.94 and 1.65 times asmassive as the Sun, respectively.[10] The tertiary member, component C, lies at anangular separation of 11.0 arc seconds from the other members.[2] It has an apparent magnitude of 8.02[2] and is itself a close binary, comprising two stars with an orbital period around 0.82 days,[7] each with an apparent magnitude of 8.75.[2]

References

[edit]
  1. ^abcdvan Leeuwen, F. (2007), "Validation of the new Hipparcos reduction",Astronomy and Astrophysics,474 (2):653–664,arXiv:0708.1752,Bibcode:2007A&A...474..653V,doi:10.1051/0004-6361:20078357,S2CID 18759600.
  2. ^abcdefghijklmTokovinin, Andrei (2018-03-01), "The Updated Multiple Star Catalog",The Astrophysical Journal Supplement Series,235 (1): 6,arXiv:1712.04750,Bibcode:2018ApJS..235....6T,doi:10.3847/1538-4365/aaa1a5,ISSN 0067-0049.Iota' Normae's database entry atVizieR.
  3. ^abcdVallenari, A.; et al. (Gaia collaboration) (2023),"Gaia Data Release 3. Summary of the content and survey properties",Astronomy and Astrophysics,674: A1,arXiv:2208.00211,Bibcode:2023A&A...674A...1G,doi:10.1051/0004-6361/202243940,S2CID 244398875. Gaia DR3 record for this source atVizieR.
  4. ^abcEdwards, T. W. (April 1976), "MK classification for visual binary components",Astronomical Journal,81:245–249,Bibcode:1976AJ.....81..245E,doi:10.1086/111879
  5. ^abSamus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017), "General catalogue of variable stars: Version GCVS 5.1",Astronomy Reports,61 (1):80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,ISSN 1063-7729,S2CID 255195566.
  6. ^de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: 14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
  7. ^abcdefTokovinin, Andrei (2025-07-09),"Spectroscopic Orbits of Subsystems in Multiple Stars. XI",The Astronomical Journal,170 (3): 143,arXiv:2507.07233,Bibcode:2025AJ....170..143T,doi:10.3847/1538-3881/adee23.
  8. ^Tokovinin, Andrei; et al. (August 2015), "Speckle Interferometry at SOAR in 2014",The Astronomical Journal,150 (2): 17,arXiv:1506.05718,Bibcode:2015AJ....150...50T,doi:10.1088/0004-6256/150/2/50,S2CID 30737411, 50.
  9. ^"iot01 Nor",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2017-08-12.
  10. ^abMalkov, O. Yu.; et al. (2012), "Dynamical masses of a selected sample of orbital binaries",Astronomy & Astrophysics,546: A69,Bibcode:2012A&A...546A..69M,doi:10.1051/0004-6361/201219774.
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