Betelgez
Betelgez (α Ori) je druga najsjajnija zvezda sazvežđa Orion [18] i deveta najsvetlija zvezda na noćnom nebu. Udaljenost od Zemlje je 643 ± 146 svetlosnih godina (197 ± 45 parseka). Prečnik Betelgeza iznosi oko 1,4 milijarde kilometara (oko 1.000 Sunčevih prečnika, više od Jupiterove orbite). Prema trenutno dostupnim podacima, naučnici smatraju da će Betelgez za oko milion godina eksplodirati u supernovu, i da će na noćnom nebu Zemlje tokom nekoliko sedmica svetleti intezitetom punog Meseca.[19]
Položaj na nebu Epoha J2000.0 Ravnodnevnica J2000.0 | |
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Sazvežđe | Orion |
Izgovor | /ˈbɛtəldʒuːz, ˈbiːtəl-, -dʒuːs/[1][2] |
Rektascenzija | 05h 55m 10.30536s[3] |
Deklinacija | +07° 24′ 25.4304″[3] |
Karakteristike | |
Evolucioni stupanj | Crveni superdžin |
Spektralni tip | M1–M2 Ia–ab[4] |
Prividna magnituda (V) | 0.50[5] (0.0–1.3[6]) |
Prividna magnituda (J) | −3.00[7] |
Prividna magnituda (K) | −4.05[7] |
U−B indeks boja | +2.06[5] |
B−V indeks boja | +1.85[5] |
Varijabilni tip | SRc[6] |
Astrometrija | |
Radijalna brzina (Rv) | +21.91[8] km/s |
Sopstveno kretanje (μ) | RA: 26.42 ± 0.25[9] mas/g Dek.: 9.60 ± 0.12[9] mas/g |
Paralaksa (π) | 4.51 ± 0.80[9] mas |
Rastojanje | +48 −34 222[9] pc |
Apsolutna magnituda (MV) | −5.85[10] |
Detalji | |
Masa | +5,0 −3,9 11,6[11] M☉ |
Poluprečnik | 887 ± 203,[12] ±217 955[11] R☉ |
Luminoznost | 000 – 90000 150[13] L☉ |
Površinska gravitacija (log g) | −0.5[14] cgs |
Temperatura | 3590[11][15] K |
Metaličnost [Fe/H] | +0.05[16] dex |
Rotaciona brzina (v sin i) | 5[17] km/s |
Starost | 8.0–8.5[12] Myr |
Druge oznake | |
Referentne baze podataka | |
SIMBAD | data |
Uticaj na kulturu uredi
Likovi Ford Prefekt i Zaphod Biblbroks iz Autostoperskog vodiča kroz galaksiju, romana Daglasa Adamsa, dolaze sa sveta „iz okoline Betelgeza“.
Imena uredi
Arapski nazivi:
- al-Jauzā / الجوزاء :Ovo je žensko ime starih arapskih legendi.
Engleski:
- Betelgeuse
Japanu:
- Heike-boši / 平家星 (Zvezda Heike klanova): Crvena zastava Heike klanova.
Procene ugaonih prečnika uredi
Ova tabela sadrži delimični spisak ugaonih merenja sprovedenih od 1920. godine. Takođe je uključena i kolona koja pruža trenutni opseg poluprečnika za svaku studiju na osnovu Betelgezove najnovije procene udaljenosti (Harper et al.) of 197 ± 45 pc.
Članak | Godina[a] | Teleskop | # | Spektar | λ (μm) | ∅ (mas)[b] | Poluprečnici[v] @ 197±45 pc |
Napomene |
---|---|---|---|---|---|---|---|---|
Michelson[20] | 1920 | Maunt Vilson | 1 | Vidljivi | 0,575 | 47,0 ± 4,7 | 3,2–6,3 AJ | Ivično zatamnjenje +17% = 55,0 |
Bonneau[21] | 1972 | Palomar | 8 | Vidljivi | 0,422–0,719 | 52,0–69,0 | 3,6–9,2 AJ | Jaka korelacija ∅ sa λ |
Balega[22] | 1978 | ESO | 3 | Vidljivi | 0,405–0,715 | 45,0–67,0 | 3,1–8,6 AJ | Nema korelacije ∅ sa λ |
1979 | SAO | 4 | Vidljivi | 0,575–0,773 | 50,0–62,0 | 3,5–8,0 AJ | ||
Buscher[23] | 1989 | WHT | 4 | Vidljivi | 0,633–0,710 | 54,0–6,10 | 4,0–7,9 AJ | Otrivene asimetrije |
Wilson[24] | 1991 | WHT | 4 | Vidljivi | 0,546–0,710 | 49,0–57,0 | 3,5–7,1 AJ | Potvrda žarišta |
Tuthill[25] | 1993 | WHT | 8 | Vidljivi | 0,633–0,710 | 43,5–54,2 | 3,2–7,0 AJ | Proučavanje žarišta na 3 zvezde |
1992 | WHT | 1 | NIR | 0.902 | 42,6 ± 0:03 | 3,0–5,6 AJ | ||
Gilliland[26] | 1995 | HST | UV | 0,24–0,27 | 104–112 | 10,3–11,1 | FWHM prečnici | |
0,265–0,295 | 92–100 | 9,1–9,8 | ||||||
Weiner[27] | 1999 | ISI | 2 | MIR (N traka) | 11,150 | 54,7 ± 0,3 | 4,1–6,7 AJ | Ivično zatamnjenje = 55,2 ± 0,5 |
Perrin[28] | 1997 | IOTA | 7 | NIR (K traka) | 2,200 | 43,33 ± 0,04 | 3,3–5,2 AJ | K i L trake, 11,5 μm kontrast podataka |
Haubois[29] | 2005 | IOTA | 6 | NIR (H traka) | 1.650 | 44,28 ± 0,15 | 3,4–5,4 AJ | Roseldov prečnik 45,03 ± 0,12 |
Hernandez[30] | 2006 | VLTI | 2 | NIR (K traka) | 2,099–2,198 | 42:57 ± 0:02 | 3,2–5,2 AJ | AMBER rezultati visoke preciznosti. |
Ohnaka[31] | 2008 | VLTI | 3 | NIR (K traka) | 2,280–2,310 | 43,19 ± 0,03 | 3,3–5,2 AJ | Ivično zatamnjenje 43,56 ± 0,06 |
Townes[32] | 1993 | ISI | 17 | MIR (H traka) | 11,150 | 56,00 ± 1,00 | 4,2–6,8 AJ | Sistematska studija koja obuhvata 17 merenja na istoj talasnoj dužini od 1993. do 2009. godine |
2008 | ISI | MIR (N traka) | 11,150 | 47,00 ± 2,00 | 3,6–5,7 AJ | |||
2009 | ISI | MIR (N traka) | 11,150 | 48,00 ± 1,00 | 3,6–5,8 AJ | |||
Ohnaka[33] | 2011 | VLTI | 3 | NIR (K traka) | 2,280–2,310 | 42,05 ± 0,05 | 3,2–5.2 AJ | Ivično zatamnjenje 42,49 ± 0,06 |
Harper[10] | 2008 | VLA | Takođe je vredno pomena da Harper et al. u zaključku njihove publikacije iznose sledeću napomenu: „U izvesnom smislu, izvedena udaljenost od 200 pc je ravnoteža između 131 pc (425 ly) Hiparkos udaljenosti i radij koji teže ka 250 pc (815 ly)” - stoga uspostavljaju ± 815 ly kao spoljne udaljenosti za zvezdu. |
Vidi još uredi
Reference uredi
- ^ Simpson, J.; Weiner, E., ur. (1989). „Betelgeuse”. Oxford English Dictionary (2nd izd.). Oxford: Clarendon Press. str. 130. ISBN 978-0-19-861186-8.
- ^ „Merriam-Webster Dictionary: Betelgeuse”. Pristupljeno 23. 4. 2018.
- ^ a b van Leeuwen, F (novembar 2007). „Hipparcos, the New Reduction”. Astronomy and Astrophysics. VizieR. 474 (2): 653—664. Bibcode:2007A&A...474..653V. arXiv:0708.1752 . doi:10.1051/0004-6361:20078357.
- ^ Keenan, Philip C.; McNeil, Raymond C. (1989). „The Perkins catalog of revised MK types for the cooler stars”. Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- ^ a b v Nicolet, B. (1978). „Catalogue of Homogeneous Data in the UBV Photoelectric Photometric System”. Astronomy & Astrophysics. 34: 1—49. Bibcode:1978A&AS...34....1N.
- ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). „VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)”. VizieR On-line Data Catalog: B/Gcvs. Originally Published In: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
- ^ a b 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.
- ^ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). „Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters”. Astronomy and Astrophysics. 430: 165—186. Bibcode:2005A&A...430..165F. arXiv:astro-ph/0409579 . doi:10.1051/0004-6361:20041272.
- ^ a b v g Harper, G. M.; Brown, A.; Guinan, E. F.; O'Gorman, E.; Richards, A. M. S.; Kervella, P.; Decin, L. (2017). „An Updated 2017 Astrometric Solution for Betelgeuse”. The Astronomical Journal. 154 (1): 11. Bibcode:2017AJ....154...11H. arXiv:1706.06020 . doi:10.3847/1538-3881/aa6ff9.
- ^ a b Harper, Graham M.; Brown, Alexander; Guinan, Edward F. (april 2008). „A New VLA-Hipparcos Distance to Betelgeuse and its Implications” (PDF). The Astronomical Journal. 135 (4): 1430—40. Bibcode:2008AJ....135.1430H. doi:10.1088/0004-6256/135/4/1430. Pristupljeno 10. 7. 2010.
- ^ a b v Neilson, H. R.; Lester, J. B.; Haubois, X. (decembar 2011). Weighing Betelgeuse: Measuring the Mass of α Orionis from Stellar Limb-darkening. 9th Pacific Rim Conference on Stellar Astrophysics. Proceedings of a conference held at Lijiang, China in 14–20 April 2011. ASP Conference Series. Astronomical Society of the Pacific. 451. str. 117. Bibcode:2011ASPC..451..117N. arXiv:1109.4562 .
- ^ a b Dolan, Michelle M.; Mathews, Grant J.; Lam, Doan Duc; Lan, Nguyen Quynh; Herczeg, Gregory J.; Dearborn, David S. P. (2016). „Evolutionary Tracks for Betelgeuse”. The Astrophysical Journal. 819 (1): 7. Bibcode:2016ApJ...819....7D. arXiv:1406.3143v2 . doi:10.3847/0004-637X/819/1/7.
- ^ Smith, Nathan; Hinkle, Kenneth H.; Ryde, Nils (mart 2009). „Red Supergiants as Potential Type IIn Supernova Progenitors: Spatially Resolved 4.6 μm CO Emission Around VY CMa and Betelgeuse”. The Astronomical Journal. 137 (3): 3558—3573. Bibcode:2009AJ....137.3558S. arXiv:0811.3037 . doi:10.1088/0004-6256/137/3/3558.
- ^ Lobel, Alex; Dupree, Andrea K. (2000). „Modeling the Variable Chromosphere of α Orionis” (PDF). The Astrophysical Journal. 545 (1): 454—74. Bibcode:2000ApJ...545..454L. doi:10.1086/317784. Pristupljeno 10. 7. 2010.
- ^ Harper, Graham M.; Brown, Alexander; Lim, Jeremy (april 2001). „A Spatially Resolved, Semiempirical Model for the Extended Atmosphere of α Orionis (M2 Iab)”. The Astrophysical Journal. 551 (2): 1073—98. Bibcode:2001ApJ...551.1073H. doi:10.1086/320215.
- ^ Ramírez, Solange V.; Sellgren, K.; Carr, John S.; Balachandran, Suchitra C.; et al. (jul 2000). „Stellar Iron Abundances at the Galactic Center” (PDF). The Astrophysical Journal. 537 (1): 205—20. Bibcode:2000ApJ...537..205R. arXiv:astro-ph/0002062 . doi:10.1086/309022. Pristupljeno 9. 7. 2010.
- ^ Kervella, P.; Verhoelst, T.; Ridgway, S. T.; Perrin, G.; Lacour, S.; et al. (septembar 2009). „The Close Circumstellar Environment of Betelgeuse. Adaptive Optics Spectro-imaging in the Near-IR with VLT/NACO”. Astronomy and Astrophysics. 504 (1): 115—25. Bibcode:2009A&A...504..115K. arXiv:0907.1843 . doi:10.1051/0004-6361/200912521.
- ^ Mišić, Milan, ur. (2005). Enciklopedija Britanika. A-B. Beograd: Narodna knjiga : Politika. str. 141. ISBN 86-331-2075-5.
- ^ Calla Cofield. „Dying Star Betelgeuse Keeps Its Cool ... and Astronomers Are Puzzled”. Space.com. Pristupljeno 25. 1. 2016.
- ^ Michelson, Albert Abraham; Pease, Francis G. (1921). „Measurement of the diameter of Alpha Orionis with the interferometer”. Astrophysical Journal. 53: 249—59. Bibcode:1921ApJ....53..249M. doi:10.1086/142603. „The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds”
- ^ Bonneau, D.; Labeyrie, A. (1973). „Speckle Interferometry: Color-Dependent Limb Darkening Evidenced on Alpha Orionis and Omicron Ceti”. Astrophysical Journal. 181: L1. Bibcode:1973ApJ...181L...1B. doi:10.1086/181171.
- ^ Balega, Iu.; Blazit, A.; Bonneau, D.; Koechlin, L.; Labeyrie, A.; Foy, R.. (novembar 1982). „The angular diameter of Betelgeuse”. Astronomy and Astrophysics. 115 (2): 253—56. Bibcode:1982A&A...115..253B.
- ^ Buscher, D. F.; Baldwin, J. E.; Warner, P. J.; Haniff, C. A. (1990). „Detection of a bright feature on the surface of Betelgeuse”. Monthly Notices of the Royal Astronomical Society. 245: 7. Bibcode:1990MNRAS.245P...7B.
- ^ Wilson, R. W.; Baldwin, J. E.; Buscher, D. F.; Warner, P. J. (1992). „High-resolution imaging of Betelgeuse and Mira”. Monthly Notices of the Royal Astronomical Society. 257 (3): 369—76. Bibcode:1992MNRAS.257..369W. doi:10.1093/mnras/257.3.369.
- ^ Tuthill P. G.; Haniff, C. A.; Baldwin, J. E. (mart 1997). „Hotspots on late-type supergiants”. Monthly Notices of the Royal Astronomical Society. 285 (3): 529—39. Bibcode:1997MNRAS.285..529T. doi:10.1093/mnras/285.3.529.
- ^ Gilliland, Ronald L.; Dupree, Andrea K. (maj 1996). „First Image of the Surface of a Star with the Hubble Space Telescope” (PDF). Astrophysical Journal Letters. 463 (1): L29. Bibcode:1996ApJ...463L..29G. doi:10.1086/310043. Pristupljeno 1. 8. 2010. „The yellow/red "image" or "photo" of Betelgeuse commonly seen is not a picture of the red supergiant, but a mathematically generated image based on the photograph. The photograph was of much lower resolution: The entire Betelgeuse image fit within a 10x10 pixel area on the Hubble Space Telescopes Faint Object Camera. The images were oversampled by a factor of 5 with bicubic spline interpolation, then deconvolved.”
- ^ Weiner, J.; Danchi, W. C.; Hale, D. D. S.; McMahon, J.; et al. (decembar 2000). „Precision Measurements of the Diameters of α Orionis and ο Ceti at 11 Microns” (PDF). The Astrophysical Journal. 544 (2): 1097—1100. Bibcode:2000ApJ...544.1097W. doi:10.1086/317264. Pristupljeno 23. 6. 2007.
- ^ Perrin, G.; Ridgway, S. T.; Coudé du Foresto, V.; Mennesson, B.; Traub, W. A.; Lacasse, M. G. (2004). „Interferometric Observations of the Supergiant Stars α Orionis and α Herculis with FLUOR at IOTA”. Astronomy and Astrophysics. 418 (2): 675—85. Bibcode:2004A&A...418..675P. arXiv:astro-ph/0402099 . doi:10.1051/0004-6361:20040052. „Assuming a distance of 197 ± 45 pc, an angular distance of 43.33 ± 0.04 mas would equate to a radius of 4.3 AU or 920 R☉”
- ^ Haubois, X.; Perrin, G.; Lacour, S.; Verhoelst, T.; Meimon, S.; et al. (2009). „Imaging the Spotty Surface of Betelgeuse in the H Band”. Astronomy & Astrophysics. 508 (2): 923—32. Bibcode:2009A&A...508..923H. arXiv:0910.4167 . doi:10.1051/0004-6361/200912927.
- ^ Hernandez Utrera, O.; Chelli, A (2009). „Accurate Diameter Measurement of Betelgeuse Using the VLTI/AMBER Instrument” (PDF). Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias). 37: 179—80. Bibcode:2009RMxAC..37..179H.
- ^ A. P. Ohnaka, K.; Hofmann, K.-H.; Benisty, M.; Chelli, A.; et al. (2009). „Spatially Resolving the Inhomogeneous Structure of the Dynamical Atmosphere of Betelgeuse with VLTI/AMBER”. Astronomy & Astrophysics. 503 (1): 183—95. Bibcode:2009A&A...503..183O. arXiv:0906.4792 . doi:10.1051/0004-6361/200912247.
- ^ Townes, C. H.; Wishnow, E. H.; Hale, D. D. S.; Walp, B. (2009). „A Systematic Change with Time in the Size of Betelgeuse” (PDF). The Astrophysical Journal Letters. 697 (2): L127—28. Bibcode:2009ApJ...697L.127T. doi:10.1088/0004-637X/697/2/L127.
- ^ Ohnaka, K.; Weigelt, G.; Millour, F.; Hofmann, K.-H.; Driebe, T.; Schertl, D.; Chelli, A.; Massi, F.; Petrov, R.; Stee, Ph. (2011). „Imaging the dynamical atmosphere of the red supergiant Betelgeuse in the CO first overtone lines with VLTI/AMBER”. Astronomy & Astrophysics. 529: A163. Bibcode:2011A&A...529A.163O. arXiv:1104.0958 . doi:10.1051/0004-6361/201016279. „We derive a uniform-disk diameter of 42.05 ± 0.05 mas and a power-law-type limb-darkened disk diameter of 42.49 ± 0.06 mas and a limb-darkening parameter of (9.7 ± 0.5) × 10−2”
Spoljašnje veze uredi
- Surface imaging of Betelgeuse with COAST and the WHT
- Near, Mid and Far Infrared
- Astronomy Picture of the Day slike: