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44 Boötis

April 12, 2024

This article is about i Boötis. It is not to be confused with ι Boötis.

44 Boötis or i Boötis is a triple star system in the constellation Boötes. It is approximately 41.6 light years from Earth.

44 Boötis

A light curve for 44 Boötis plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension 15h 03m 47.29565s[2]
Declination +47° 39′ 14.6228″[2]
Apparent magnitude (V) 4.70 - 4.84[3] (5.136 / 6.004)[4]
Characteristics
Spectral type G0Vnv[5] + (K0V + K4V)[6]
U−B color index 0.09[7]
B−V color index 0.65[7]
Variable type W UMa[3]
Astrometry
Radial velocity (Rv)−17.89[8] km/s
Proper motion (μ) RA: −445.84[2] mas/yr
Dec.: 19.86[2] mas/yr
Parallax (π)78.39 ± 1.03 mas[9]
Distance41.6 ± 0.5 ly
(12.8 ± 0.2 pc)
Absolute magnitude (MV)+2.211[9] / +5.38[10]
Orbit[11]
Primary44 Boo A
Companion44 Boo B
Period (P)209.8±3.3 yr
Semi-major axis (a)3.666±0.021″
Eccentricity (e)0.5111±0.0065
Inclination (i)83.55±0.05°
Longitude of the node (Ω)57.14±0.06°
Periastron epoch (T)B 2012.04±0.26
Argument of periastron (ω)
(secondary)		39.86±0.68°
Orbit[10]
Primary44 Boo Ba
Companion44 Boo Bb
Period (P)0.267818 days
Semi-major axis (a)2.015 R☉
Eccentricity (e)0.0
Inclination (i)72.8°
Semi-amplitude (K1)
(primary)		231.31 km/s
Semi-amplitude (K2)
(secondary)		112.70 km/s
Details
44 Boo A
Mass1.04±0.10[11] M☉
Luminosity1.552[4] L☉
Surface gravity (log g)4.33[12] cgs
Temperature5,877[12] K
Metallicity [Fe/H]−0.24[12] dex
Age1.4–1.5[13] Gyr
44 Boo BA
Mass0.98[14] M☉
Radius0.87[14] R☉
Luminosity0.51[14] L☉
Temperature5,300[14] K
44 Boo Bb
Mass0.55[14] M☉
Radius0.66[14] R☉
Luminosity0.24[14] L☉
Temperature5,035[14] K
Other designations
i Boötis, 40 Boo, BD+48°2259, FK5 3182, GJ 575, HD 133640, HIP 73695, HR 5618, SAO 45357, ADS 9494, CCDM 15038+4739[15]
Database references
SIMBADdata
A
B

44 Boötis can be resolved into two stars, of 5th and 6th magnitudes respectively. They were separated by 1.5″ when the pair were confirmed in 1819, but were only 0.2″ by 2020 as the two orbit every 210 years.[16][11]

The primary component, 44 Boötis A, is a yellow-white G-type main sequence dwarf with a mean apparent magnitude of +4.83. The companion component, 44 Boötis B, is a W Ursae Majoris variable spectroscopic binary. The variability of this star system was discovered by English astronomer William Herschel.[17] The brightness of the eclipsing binary varies from magnitude +5.8 to +6.40 with a period of 6.43 hours.[18] The two eclipsing components of the system are close enough to allow their stellar envelopes to overlap, or at least nearly so.[10] In 1948, flare behavior was measured from this system based on data from O. J. Eggen.[19]

The 44 Boötis system is 42 light-years (13 parsecs) from Earth.[9] It also may show signs of an infrared excess, implying the existence of a dust disk that absorbs visible light and re-emits it as infrared light. The dust would have a blackbody temperature of about 23 K, situated up to 182 au from the parent star.[4]

References edit

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d van Leeuwen, F. (November 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.
  3. ^ a b Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ^ a b c Montesinos, B.; et al. (September 2016). "Incidence of debris discs around FGK stars in the solar neighbourhood". Astronomy & Astrophysics. 593: 31. arXiv:1605.05837. Bibcode:2016A&A...593A..51M. doi:10.1051/0004-6361/201628329. S2CID 55251562. A51.
  5. ^ Gray, R. O.; Napier, M. G.; Winkler, L. I. (April 2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal. 121 (4): 2148–2158. Bibcode:2001AJ....121.2148G. doi:10.1086/319956.
  6. ^ Zasche, P.; Wolf, M.; Hartkopf, W. I.; Svoboda, P.; Uhlař, R.; Liakos, A.; Gazeas, K. (2009). "A Catalog of Visual Double and Multiple Stars with Eclipsing Components". The Astronomical Journal. 138 (2): 664. arXiv:0907.5172. Bibcode:2009AJ....138..664Z. doi:10.1088/0004-6256/138/2/664. S2CID 17089387.
  7. ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. SIMBAD. Bibcode:1986EgUBV........0M.
  8. ^ Bilir, S.; et al. (February 2005). "Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation". Monthly Notices of the Royal Astronomical Society. 357 (2): 497–517. arXiv:astro-ph/0411291. Bibcode:2005MNRAS.357..497B. doi:10.1111/j.1365-2966.2005.08609.x. S2CID 16274339.
  9. ^ a b c Eker, Z.; et al. (2009). "New absolute magnitude calibrations for W Ursa Majoris type binaries". Astronomische Nachrichten. 330 (1): 68–77. arXiv:0807.4989. Bibcode:2009AN....330...68E. doi:10.1002/asna.200811041. S2CID 15071352.
  10. ^ a b c Lu, Wenxian; Rucinski, Slavek M; Ogłoza, Waldemar (2001). "Radial Velocity Studies of Close Binary Stars. IV". The Astronomical Journal. 122 (1): 402–412. arXiv:astro-ph/0104065. Bibcode:2001AJ....122..402L. doi:10.1086/321131. S2CID 118866197.
  11. ^ a b c Zirm, Henry (2011). "The Rapid Convergence of 44 Boötis with Revised Orbit and Updated Ephemerides" (PDF). Journal of Double Star Observations. 7 (1): 24–36. Bibcode:2011JDSO....7...24Z.
  12. ^ a b c Ramírez, I.; et al. (September 2012). "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets". The Astrophysical Journal. 756 (1): 46. arXiv:1207.0499. Bibcode:2012ApJ...756...46R. doi:10.1088/0004-637X/756/1/46. S2CID 119199829.
  13. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  14. ^ a b c d e f g h Latković, Olivera; Čeki, Atila; Lazarević, Sanja (2021). "Statistics of 700 Individually Studied W UMa Stars". The Astrophysical Journal Supplement Series. 254 (1): 10. arXiv:2103.06693. Bibcode:2021ApJS..254...10L. doi:10.3847/1538-4365/abeb23. S2CID 232185576.
  15. ^ "* i Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2015-04-22.
  16. ^ Mason, Brian D.; et al. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  17. ^ Percy, John R. (2007). Understanding Variable Stars. Cambridge University Press. p. 3. ISBN 978-1139463287.
  18. ^ Malkov, O. Yu.; et al. (2006). "A catalogue of eclipsing variables". Astronomy and Astrophysics. 446 (2): 785–89. Bibcode:2006A&A...446..785M. doi:10.1051/0004-6361:20053137. hdl:10995/73280.
  19. ^ Huruhata, Masaaki (August 1952). "Flaring Phenomena in U Pegasi". Publications of the Astronomical Society of the Pacific. 64 (379): 200. Bibcode:1952PASP...64..200H. doi:10.1086/126463.

External links edit

  • HR 5618
  • Image 44 Boötis
  • CCDM J15038+4739

April 12, 2024
boötis, this, article, about, boötis, confused, with, boötis, boötis, triple, star, system, constellation, boötes, approximately, light, years, from, earth, light, curve, plotted, from, tess, data, observation, dataepoch, j2000, equinox, j2000constellation, bo. This article is about i Bootis It is not to be confused with i Bootis 44 Bootis or i Bootis is a triple star system in the constellation Bootes It is approximately 41 6 light years from Earth 44 BootisA light curve for 44 Bootis plotted from TESS data 1 Observation dataEpoch J2000 Equinox J2000Constellation BootesRight ascension 15h 03m 47 29565s 2 Declination 47 39 14 6228 2 Apparent magnitude V 4 70 4 84 3 5 136 6 004 4 CharacteristicsSpectral type G0Vnv 5 K0V K4V 6 U B color index 0 09 7 B V color index 0 65 7 Variable type W UMa 3 AstrometryRadial velocity Rv 17 89 8 km sProper motion m RA 445 84 2 mas yr Dec 19 86 2 mas yrParallax p 78 39 1 03 mas 9 Distance41 6 0 5 ly 12 8 0 2 pc Absolute magnitude MV 2 211 9 5 38 10 Orbit 11 Primary44 Boo ACompanion44 Boo BPeriod P 209 8 3 3 yrSemi major axis a 3 666 0 021 Eccentricity e 0 5111 0 0065Inclination i 83 55 0 05 Longitude of the node W 57 14 0 06 Periastron epoch T B 2012 04 0 26Argument of periastron w secondary 39 86 0 68 Orbit 10 Primary44 Boo BaCompanion44 Boo BbPeriod P 0 267818 daysSemi major axis a 2 015 R Eccentricity e 0 0Inclination i 72 8 Semi amplitude K1 primary 231 31 km sSemi amplitude K2 secondary 112 70 km sDetails44 Boo AMass1 04 0 10 11 M Luminosity1 552 4 L Surface gravity log g 4 33 12 cgsTemperature5 877 12 KMetallicity Fe H 0 24 12 dexAge1 4 1 5 13 Gyr44 Boo BAMass0 98 14 M Radius0 87 14 R Luminosity0 51 14 L Temperature5 300 14 K44 Boo BbMass0 55 14 M Radius0 66 14 R Luminosity0 24 14 L Temperature5 035 14 KOther designationsi Bootis 40 Boo BD 48 2259 FK5 3182 GJ 575 HD 133640 HIP 73695 HR 5618 SAO 45357 ADS 9494 CCDM 15038 4739 15 Database referencesSIMBADdataAB44 Bootis can be resolved into two stars of 5th and 6th magnitudes respectively They were separated by 1 5 when the pair were confirmed in 1819 but were only 0 2 by 2020 as the two orbit every 210 years 16 11 The primary component 44 Bootis A is a yellow white G type main sequence dwarf with a mean apparent magnitude of 4 83 The companion component 44 Bootis B is a W Ursae Majoris variable spectroscopic binary The variability of this star system was discovered by English astronomer William Herschel 17 The brightness of the eclipsing binary varies from magnitude 5 8 to 6 40 with a period of 6 43 hours 18 The two eclipsing components of the system are close enough to allow their stellar envelopes to overlap or at least nearly so 10 In 1948 flare behavior was measured from this system based on data from O J Eggen 19 The 44 Bootis system is 42 light years 13 parsecs from Earth 9 It also may show signs of an infrared excess implying the existence of a dust disk that absorbs visible light and re emits it as infrared light The dust would have a blackbody temperature of about 23 K situated up to 182 au from the parent star 4 References edit MAST Barbara A Mikulski Archive for Space Telescopes Space Telescope Science Institute Retrieved 8 December 2021 a b c d van Leeuwen F November 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b Samus N N Kazarovets E V Durlevich O V Kireeva N N Pastukhova E N 2017 General catalogue of variable stars Version GCVS 5 1 Astronomy Reports 61 1 80 Bibcode 2017ARep 61 80S doi 10 1134 S1063772917010085 S2CID 125853869 a b c Montesinos B et al September 2016 Incidence of debris discs around FGK stars in the solar neighbourhood Astronomy amp Astrophysics 593 31 arXiv 1605 05837 Bibcode 2016A amp A 593A 51M doi 10 1051 0004 6361 201628329 S2CID 55251562 A51 Gray R O Napier M G Winkler L I April 2001 The Physical Basis of Luminosity Classification in the Late A F and Early G Type Stars I Precise Spectral Types for 372 Stars The Astronomical Journal 121 4 2148 2158 Bibcode 2001AJ 121 2148G doi 10 1086 319956 Zasche P Wolf M Hartkopf W I Svoboda P Uhlar R Liakos A Gazeas K 2009 A Catalog of Visual Double and Multiple Stars with Eclipsing Components The Astronomical Journal 138 2 664 arXiv 0907 5172 Bibcode 2009AJ 138 664Z doi 10 1088 0004 6256 138 2 664 S2CID 17089387 a b Mermilliod J C 1986 Compilation of Eggen s UBV data transformed to UBV unpublished Catalogue of Eggen s UBV Data SIMBAD Bibcode 1986EgUBV 0M Bilir S et al February 2005 Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation Monthly Notices of the Royal Astronomical Society 357 2 497 517 arXiv astro ph 0411291 Bibcode 2005MNRAS 357 497B doi 10 1111 j 1365 2966 2005 08609 x S2CID 16274339 a b c Eker Z et al 2009 New absolute magnitude calibrations for W Ursa Majoris type binaries Astronomische Nachrichten 330 1 68 77 arXiv 0807 4989 Bibcode 2009AN 330 68E doi 10 1002 asna 200811041 S2CID 15071352 a b c Lu Wenxian Rucinski Slavek M Ogloza Waldemar 2001 Radial Velocity Studies of Close Binary Stars IV The Astronomical Journal 122 1 402 412 arXiv astro ph 0104065 Bibcode 2001AJ 122 402L doi 10 1086 321131 S2CID 118866197 a b c Zirm Henry 2011 The Rapid Convergence of 44 Bootis with Revised Orbit and Updated Ephemerides PDF Journal of Double Star Observations 7 1 24 36 Bibcode 2011JDSO 7 24Z a b c Ramirez I et al September 2012 Lithium Abundances in nearby FGK Dwarf and Subgiant Stars Internal Destruction Galactic Chemical Evolution and Exoplanets The Astrophysical Journal 756 1 46 arXiv 1207 0499 Bibcode 2012ApJ 756 46R doi 10 1088 0004 637X 756 1 46 S2CID 119199829 Mamajek Eric E Hillenbrand Lynne A November 2008 Improved Age Estimation for Solar Type Dwarfs Using Activity Rotation Diagnostics The Astrophysical Journal 687 2 1264 1293 arXiv 0807 1686 Bibcode 2008ApJ 687 1264M doi 10 1086 591785 S2CID 27151456 a b c d e f g h Latkovic Olivera Ceki Atila Lazarevic Sanja 2021 Statistics of 700 Individually Studied W UMa Stars The Astrophysical Journal Supplement Series 254 1 10 arXiv 2103 06693 Bibcode 2021ApJS 254 10L doi 10 3847 1538 4365 abeb23 S2CID 232185576 i Boo SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2015 04 22 Mason Brian D et al December 2001 The 2001 US Naval Observatory Double Star CD ROM I The Washington Double Star Catalog The Astronomical Journal 122 6 3466 3471 Bibcode 2001AJ 122 3466M doi 10 1086 323920 Percy John R 2007 Understanding Variable Stars Cambridge University Press p 3 ISBN 978 1139463287 Malkov O Yu et al 2006 A catalogue of eclipsing variables Astronomy and Astrophysics 446 2 785 89 Bibcode 2006A amp A 446 785M doi 10 1051 0004 6361 20053137 hdl 10995 73280 Huruhata Masaaki August 1952 Flaring Phenomena in U Pegasi Publications of the Astronomical Society of the Pacific 64 379 200 Bibcode 1952PASP 64 200H doi 10 1086 126463 External links editHR 5618 Image 44 Bootis CCDM J15038 4739 Retrieved from https en wikipedia org w index php title 44 Bootis amp oldid 1206414954, wikipedia, wiki, book, books, library,

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