قلب‌العقرب

از ویکی‌پدیا، دانشنامهٔ آزاد
پرش به ناوبری پرش به جستجو
فارسیEnglish

مختصات: نقشه آسمان ۱۶h ۲۹m ۲۴s٬ −۲۶° ۲۵′ ۵۵″


قلب عقرب A/B

Antares 3° region on DSS2 all sky survey
اطلاعات رصدی
مبدا مبدأ (ستاره‌شناسی)      اعتدال مبدأ (ستاره‌شناسی)
صورت فلکی عقرب
بعد 16h 29m 24s[۱]
میل ‏ 55″ 25′ ‎−26°[۱]
قدر ظاهری (V)1.09[۱]
مشخصات
ردهM1.5Iab-b / B2.5V[۱]
راهنمای رنگ U-B۱٫۳۴
راهنمای رنگ B-V۱٫۸۷
اخترسنجی
سرعت شعاعی (Rv)−3.4[۱] km/s
حرکت مخصوص (μ) RA: −10.16[۱] mas/yr
Dec.: −23.21[۱] mas/yr
اختلاف منظر (π)۵٫۴۰ ± ۱٫۶۸[۱] mas
جزئیات
جرم۱۵٫۵ M
درخشندگی۶۵٬۰۰۰(بولومتریک) L
دما۳٬۵۰۰ K
نام‌گذاری‌های دیگر
آلفا عقرب، [۱] 21 Sco,[۱] Cor Scorpii, Kalb al بتا کژدم، Scorpion's Heart, Vespertilio, HR 6134,[۱] CD -26°11359,[۱] HD 148478,[۱] SAO 184415,[۱] FK5 616,[۱] WDS 16294-2626, CCDM J16294-2626A/B,[۱] HIP 80763.[۱]
منابع
سیمباداطلاعات

قَلب‌العَقرَب، کژدم‌دل یا سَدویس (به انگلیسی: Antares یا Alpha Scorpii) درخشان‌ترین ستارهٔ صورت فلکی کژدم است. قلب عقرب یک ابرغول سرخ و یکی از درخشان‌ترین ستاره‌های آسمان است. این ستاره احتمالاً از سال ۱۵۰ میلادی این‌گونه درخشان است چرا که در سال ۲۰۰ پ.م. آن را کم‌نورتر از ستاره کفه شمالی[۲] توصیف کرده‌اند.

توصیف پیشینیان[ویرایش]

اقرب‌الموارد می‌نویسد: قلب‌العقرب ستاره‌ای است نورانی و در کنار آن دو ستاره است. صبح‌الاعشی ج ۲ ص ۱۶۰ می‌نویسد: یکی از ستارگان منازل قمر است، و آن ستاره‌ای است قرمز و نورانی در میان دو ستاره کم نور که عربان آن دو را «نیاطی القلب» خوانند و اصحاب صور این ستاره را قلب گویند از آنجا که در موضع قلب از صورت عقرب قرار دارد؛ و قلوب چهار ستاره‌اند: یکی همین قلب‌العقرب، دوم قلب‌السمکه، سوم قلب‌الثور، چهارم قلب‌الاسد، و هر جا قلب به طور اطلاق و بدون اضافه ذکر شود مراد قلب العقرب است.[۳]

اسطوره ستاره‌شناسی[ویرایش]

در اسطوره‌های ایرانی و زرتشتی، ستاره کژدم‌دل نماد اپوش، دیو خشکی شناخته می‌شود که با تیشتر، ایزد باران و باروری خاک در نبرد است. ستاره نماد ایزدتیشتر، شباهنگ است که درخشان‌ترین ستاره آسمان شب در آسمان ایران‌زمین است.

جستارهای وابسته[ویرایش]

هم‌سنجی سیاره‌های منظومه خورشیدی با تعدادی از ستاره‌های مشهور:
الف:
زمین (۴) > ناهید (۳) > مریخ (۲) > تیر (۱)
ب:
مشتری (۸) > زحل (۷) > اورانوس(۶) > نپتون (۵) > زمین (بدون شماره)
پ:
شباهنگ (۱۱) > خورشید (۱۰) > ولف ۳۵۹ (۹) > مشتری (بدون شماره)
ت:
دبران (۱۴) > نگهبان شمال (۱۳) > رأس پیکر پسین (۱۲) > شباهنگ (بدون شماره)
ث:
ابط‌الجوزا (۱۷) >قلب عقرب (۱۶) > پای شکارچی (۱۵) > دبران (بدون شماره)
ج:
وی‌وای سگ بزرگ (۲۰) >وی‌وی قیفاووس (۱۹) > مو قیفاووس (۱۸) > ابط‌الجوزا (بدون شماره)

منابع[ویرایش]

*منبع اطلاعات جدول: Bright Star Catalogue.

  • Wikipedia-bijdragers, "Antares," Wikipedia, de vrije encyclopedie, (accessed januari 31, 2008).
  • بهار، مهرداد، پژوهشی در اساطیر ایران، تهران: چاپ سوم ۱۳۷۸ خ.
  1. ۱٫۰۰ ۱٫۰۱ ۱٫۰۲ ۱٫۰۳ ۱٫۰۴ ۱٫۰۵ ۱٫۰۶ ۱٫۰۷ ۱٫۰۸ ۱٫۰۹ ۱٫۱۰ ۱٫۱۱ ۱٫۱۲ ۱٫۱۳ ۱٫۱۴ ۱٫۱۵ ۱٫۱۶ SIMBAD Astronomical Database (Results for CCDM J16294-2626A/B ed.) Retrieved on 2006-10-23.
  2. (Zuben-el-schemali)، زُبن شمالی نام عربی آنست که به زبان‌های اروپایی رفته. زُبن در عربی به معنی چنگال (عقرب) است.[۱] منظور از کفه در فارسی کفهٔ شمالی ترازو است.
  3. دهخدا

Antares
Scorpius IAU.svg
Antares is near the center of the constellation Scorpius
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension  16h 29m 24.45970s[1]
Declination −26° 25′ 55.2094″[1]
Apparent magnitude (V) 0.6 - 1.6[2] + 5.5[3]
Characteristics
Evolutionary stage Red supergiant
Spectral type M1.5Iab-Ib[4] + B2.5V[5]
U−B color index +1.34[3]
B−V color index +1.83[3]
Variable type Lc[2]
Astrometry
Radial velocity (Rv)−3.4[6] km/s
Proper motion (μ) RA: −12.11[1] mas/yr
Dec.: −23.30[1] mas/yr
Parallax (π)5.89 ± 1.00[1] mas
Distanceapprox. 550 ly
(approx. 170 pc)
Absolute magnitude (MV)−5.28[7] (variable)
Details
A
Mass11 - 14.3[8] M
Radius680[8]–800[9] R
Luminosity75900+53000
−31200
[10] L
Surface gravity (log g)−0.1 - −0.2[8] cgs
Temperature3,660±120[8] K
Rotational velocity (v sin i)20[3] km/s
Age15±5[8] Myr
B
Mass7.2[11] M
Radius5.2[11] R
Luminosity2,754[11] L
Surface gravity (log g)3.9[11] cgs
Temperature18,500[12] K
Rotational velocity (v sin i)250[11] km/s
Other designations
α Scorpii, 21 Sco, Cor Scorpii, Kalb al Akrab, Scorpion's Heart, Vespertilio,[13] HR 6134, CD−26°11359, HIP 80763, SAO 184415, FK5 616, WDS 16294-2626, CCDM J16294-2626
A: HD 148478, AAVSO 1623-26
B: HD 148479
Database references
SIMBADAntares
α Scorpii A
α Scorpii B

Antares /ænˈtɛərz/,[14][15] designated α Scorpii (Latinised to Alpha Scorpii, abbreviated Alpha Sco, α Sco), is on average the fifteenth-brightest star in the night sky, and the brightest object in the constellation of Scorpius. Distinctly reddish when viewed with the naked eye, Antares is a slow irregular variable star that ranges in brightness from apparent magnitude +0.6 to +1.6. Often referred to as "the heart of the scorpion", Antares is flanked by σ Scorpii and τ Scorpii near the center of the constellation.

Classified as a red supergiant of spectral type M1.5Iab-Ib, Antares is a red supergiant, a large evolved massive star. Its exact size remains uncertain, but if placed at the center of the Solar System it would reach to somewhere between the orbits of Mars and Jupiter. Its mass is calculated to be around 12 times that of the Sun.

Antares is the brightest, most massive, and most evolved stellar member of the nearest OB association, the Scorpius–Centaurus Association. Antares is a member of the Upper Scorpius subgroup of the association, which contains thousands of stars with a mean age of 11 million years, about 170 parsecs (550 ly) from Earth.

Antares appears as a single star when viewed with the naked eye, but it is actually a binary star, with its two components called α Scorpii A and α Scorpii B. The brighter of the pair is the red supergiant, while the fainter is a hot main sequence star of magnitude 5.5.

Nomenclature

Antares between σ and τ Scorpii. Antares appears white in this WISE false colour infrared image.

α Scorpii (Latinised to Alpha Scorpii) is the star's Bayer designation. Antares has the Flamsteed designation 21 Scorpii, as well as catalogue designations such as HR 6134 in the Bright Star Catalogue and HD 148478 in the Henry Draper Catalogue. As a prominent infrared source, it appears in the Two Micron All-Sky Survey catalogue as 2MASS J16292443-2625549 and the Infrared Astronomical Satellite (IRAS) Sky Survey Atlas catalogue as IRAS 16262-2619. It is also catalogued as a double star WDS J16294-2626 and CCDM J16294-2626. Antares is a variable star and is listed in the General Catalogue of Variable Stars but as a Bayer-designated star it does not have a separate variable star designation.[16]

Its traditional name Antares derives from the Ancient Greek Ἀντάρης,[17] meaning "rival to-Ares" ("opponent to-Mars"), due to the similarity of its reddish hue to the appearance of the planet Mars.[18] The comparison of Antares with Mars may have originated with early Mesopotamian astronomers.[13] Some scholars have speculated that the star may have been named after Antar, or Antarah ibn Shaddad, the Arab warrior-hero celebrated in the pre-Islamic poems Mu'allaqat.[13] In 2016, the International Astronomical Union organised a Working Group on Star Names (WGSN)[19] to catalog and standardise proper names for stars. The WGSN's first bulletin of July 2016[20] included a table of the first two batches of names approved by the WGSN, which included Antares for the star α Scorpii A. It is now so entered in the IAU Catalog of Star Names.[21]

Observation

Antares is visible all night around May 31 of each year, when the star is at opposition to the Sun. Antares then rises at dusk and sets at dawn as seen at the equator. For two to three weeks on either side of November 30 Antares is not visible in the night sky, because it is near conjunction with the Sun;[22] this period of invisibility is longer in the Northern Hemisphere than in the Southern Hemisphere, since the star's declination is south of the celestial equator.

History

Antares near the Sun on 30 November

Radial velocity variations were observed in the spectrum of Antares in the early 20th century[23] and attempts were made to derive spectroscopic orbits.[24] It became apparent that the small variations could not be due to orbital motion, and were actually caused by pulsation of the star's atmosphere. Even in 1928, it was calculated that the size of the star must vary by about 20%.[25]

Antares was first reported to have a companion star by Johann Tobias Bürg during an occultation on April 13, 1819,[26] although this was not widely accepted and dismissed as a possible atmospheric effect.[27] It was then observed by Scottish astronomer James William Grant FRSE while in India on 23 July 1844.[28] It was rediscovered by Ormsby M. Mitchel in 1846,[29] and measured by William Rutter Dawes in April 1847.[30][31]

In 1952, Antares was reported to vary in brightness. A photographic magnitude range from 3.00 to 3.16 was described.[32] The brightness has been monitored by the American Association of Variable Star Observers since 1945,[33] and it has been classified as an LC slow irregular variable star, whose apparent magnitude slowly varies between extremes of +0.6 and +1.6, although usually near magnitude +1.0. There is no obvious periodicity, but statistical analyses have suggested periods of 1,733 days or 1650±640 days.[2] No separate long secondary period has been detected,[34] although it has been suggested that primary periods longer than a thousand days are analogous to long secondary periods.[2]

Research published in 2018 demonstrated that Ngarrindjeri Aboriginal people from South Australia observed the variability of Antares and incorporated it into their oral traditions as Waiyungari (meaning 'red man').[35]

Occultations and Conjunctions

Lunar Occultation of Antares (reappearance) was observed on 2006 May 14 from The Blue Mountains, Australia. Antares B reappears first, followed by Antares A 7.53 seconds later.

Antares is 4.57 degrees south of the ecliptic, one of four first magnitude stars within 6° of the ecliptic (the others are Spica, Regulus and Aldebaran), so it can be occulted by the Moon. On 31 July 2009, Antares was occulted by the Moon. The event was visible in much of southern Asia and the Middle East.[36][37] Every year around December 2 the Sun passes 5° north of Antares.[22] Lunar occultations of Antares are fairly common, depending on the Saros cycle. The last cycle ended in 2010 and the next begins in 2023. Shown at right is a video of a reappearance event, clearly showing events for both components.

Antares can also be occulted by the planets, e.g. Venus, but these events are rare. The last occultation of Antares by Venus took place on September 17, 525 BC; the next one will be November 17, 2400.[38] Other planets have been calculated not to have occulted Antares over the last millennium, nor will they in the next millennium, as most planets stay near the ecliptic and pass north of Antares.[39] Venus will be extremely near Antares on October 19, 2117 and every eight years thereafter through to October 29, 2157 it will pass south of the star.[40]

Stellar system

α Scorpii is a double star that are thought to form a binary system. The best calculated orbit for the stars is considered to be unreliable.[41] It describes an almost circular orbit seen nearly edge-on, with a period of 1,218 years and a semi-major axis of about 2.9.[42] Other recent estimates of the period have ranged from 880 years for a calculated orbit,[43] to 2,562 years for a simple Kepler's Law estimate.[44]

Early measurements of the pair found them to be about 3.5″ apart in 1847-49,[31] or 2.5″ apart in 1848.[29] More modern observations consistently give separations around 2.6″ - 2.8″.[45][46][47][48] The variations in the separation are often interpreted as evidence of orbital motion,[29][5] but are more likely to be simply observational inaccuracies with very little true relative motion between the two components.[42]

The pair have a projected separation of about 529 astronomical units (AU) at the estimated distance of Antares, giving a minimum value for the distance between them. Spectroscopic examination of the energy states in the outflow of matter from the companion star suggests that it is over 220 AU beyond the primary.[5]

Antares

VLTI reconstructed view of the surface of Antares A

Antares is a red supergiant star with a stellar classification of M1.5Iab-Ib, and is indicated to be a spectral standard for that class.[4] Due to the nature of the star, the derived parallax measurements have large errors, so that the true distance of Antares is approximately 550 light-years (170 parsecs) from the Sun.[1]

The brightness of Antares at visual wavelengths is about 10,000 times that of the Sun, but because the star radiates a considerable part of its energy in the infrared part of the spectrum, the true bolometric luminosity is around 100,000 times that of the Sun. There is a large margin of error assigned to values for the bolometric luminosity, typically 30% or more. There is also considerable variation between values published by different authors, for example 75,900 L and 97,700 L published in 2012 and 2013.[10][8]

The mass of the star has been calculated to be about 12 M,[10] or 11 to 14.3 M.[8] Comparison of the effective temperature and luminosity of Antares to theoretical evolutionary tracks for massive stars suggest a progenitor mass of 17 M and an age of 12 million years (MYr),[10] or an initial mass of 15 M and an age of 11 to 15 MYr.[8] Massive stars like Antares are expected to explode as supernovae.[49]

Portion of a large yellow-orange circle representing Antares, with a black circle for the orbit of Mars, and images of Arcturus and the sun to scale
Comparison between the red supergiant Antares and the Sun, shown as the tiny dot toward the upper right

Like most cool supergiants, Antares's size has much uncertainty due to the tenuous and translucent nature of the extended outer regions of the star. Defining an effective temperature is difficult due to spectral lines being generated at different depths in the atmosphere, and linear measurements produce different results depending on the wavelength observed.[50] In addition, Antares appears to pulsate, varying its radius by 165 R or 19%.[10] It also varies in temperature by 150 K, lagging 70 days behind radial velocity changes which are likely to be caused by the pulsations.[51]

The diameter of Antares can be measured most accurately using interferometry or observing lunar occultations events. An apparent diameter from occultations 41.3 ± 0.1 milliarcseconds has been published.[52] Interferometry allows synthesis of a view of the stellar disc, which is then represented as a limb-darkened disk surrounded by an extended atmosphere. The diameter of the limb-darkened disk was measured as 37.38±0.06 milliarcseconds in 2009 and 37.31±0.09 milliarcseconds in 2010. The linear radius of the star can be calculated from its angular diameter and distance. However, the distance to Antares is not known with the same accuracy as modern measurements of its diameter.

The Hipparcos satellite's trigonometric parallax of 5.89±1.00 mas[53] leads to a radius of about 680 R.[8] Older radii estimates exceeding 850 R were derived from older measurements of the diameter,[51] but those measurements are likely to have been affected by asymmetry of the atmosphere and the narrow range of infrared wavelengths observed; Antares has an extended shell which radiates strongly at those particular wavelengths.[8] Despite its large size compared to the Sun, Antares is dwarfed by even larger red supergiants, such as VY Canis Majoris, which is almost 30 times larger in terms of volume, or VV Cephei A and Mu Cephei.

Antares, like the similarly-sized red supergiant Betelgeuse in the constellation Orion, will almost certainly explode as a supernova,[54] possibly in the next ten thousand years. For a few months, the Antares supernova could be as bright as the full moon and be visible in daytime.[49]

Antares B

Antares B is a magnitude 5.5 blue-white main-sequence star of spectral type B2.5V; it also has numerous unusual spectral lines suggesting it has been polluted by matter ejected by Antares.[5] It is assumed to be a relatively normal early-B main sequence star with a mass around 7 M, a temperature around 18,500 K, and a radius of about 5 R.[11]

Antares B is normally difficult to see in small telescopes due to glare from Antares, but can sometimes be seen in apertures over 150 millimetres (5.9 inches).[55] It is often described as green, but this is probably either a contrast effect,[56] or the result of the mixing of light from the two stars when they are seen together through a telescope and are too close to be completely resolved. Antares B can sometimes be observed with a small telescope for a few seconds during lunar occultations while Antares is hidden by the Moon.[26]. Antares B appears a profound blue or bluish-green color, in contrast to the orange-red Antares.[27][26][29]

Etymology and mythology

Antares seen from the ground

In the Babylonian star catalogues dating from at least 1100 BCE, Antares was called GABA GIR.TAB, "the Breast of the Scorpion". In MUL.APIN, which dates between 1100 and 700 BC, it is one of the stars of Ea in the southern sky and marks breast of the Scorpion goddess Ishhara.[57] Later names that translate as "the Heart of Scorpion" include Calbalakrab from the Arabic Qalb al-Άqrab.[58] This had been directly translated from the Ancient Greek Καρδία Σκορπίου Kardia Skorpiū. Cor Scorpii translated above Greek name into Latin.[13]

In ancient Mesopotamia, Antares may have been known by the following names: Urbat, Bilu-sha-ziri ("the Lord of the Seed"), Kak-shisa ("the Creator of Prosperity"), Dar Lugal ("The King"), Masu Sar ("the Hero and the King"), and Kakkab Bir ("the Vermilion Star").[13] In ancient Egypt, Antares represented the scorpion goddess Serket (and was the symbol of Isis in the pyramidal ceremonies).[13] It was called tms n hntt "the red one of the prow". [59]

In Persia Antares was known as Satevis, one of the four "royal stars". In India, it with σ Scorpii and τ Scorpii were Jyeshthā (the eldest or biggest, probably attributing its huge size), one of the nakshatra (Hindu lunar mansions).[13]

The ancient Chinese called Antares 心宿二 (Xīnxiù'èr, "second star of mansion Heart"), because it was the second star of the mansion Xin (心). It was the national star of the Shang Dynasty, and it was sometimes referred to as (Chinese: 火星; pinyin: Huǒxīng; literally: 'fiery star') because of its reddish appearance.

The Māori people of New Zealand call Antares Rehua, and regard it as the chief of all the stars. Rehua is father of Puanga/Puaka (Rigel), an important star in the calculation of the Māori calendar. The Wotjobaluk Koori people of Victoria, Australia, knew Antares as Djuit, son of Marpean-kurrk (Arcturus); the stars on each side represented his wives. The Kulin Kooris saw Antares (Balayang) as the brother of Bunjil (Altair).[60]

In culture

Antares appears in the flag of Brazil, which displays 27 stars, each representing a federated unit of Brazil. Antares represents the state of Piauí.

References

  1. ^ a b c d e f 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.
  2. ^ a b c d Kiss, L. L.; Szabo, G. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society. 372 (4): 1721–1734. arXiv:astro-ph/0608438. Bibcode:2006MNRAS.372.1721K. doi:10.1111/j.1365-2966.2006.10973.x. ISSN 0035-8711.
  3. ^ a b c d Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050. Bibcode:1995yCat.5050....0H. Vizier database entry CDS. Accessed on line September 07, 2012
  4. ^ a b 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.
  5. ^ a b c d Baade, R.; Reimers, D. (October 2007). "Multi-component absorption lines in the HST spectra of α Scorpii B". Astronomy and Astrophysics. 474 (1): 229–237. Bibcode:2007A&A...474..229B. doi:10.1051/0004-6361:20077308.
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Determination of Radial Velocities and Their Applications. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ Buick, Tony (2010). "Classification of the Stars". The Rainbow Sky. Patrick Moore's Practical Astronomy Series. pp. 43–71. doi:10.1007/978-1-4419-1053-0_4. ISBN 978-1-4419-1052-3. ISSN 1431-9756.
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  11. ^ a b c d e f Kudritzki, R. P.; Reimers, D. (1978). "On the absolute scale of mass-loss in red giants. II. Circumstellar absorption lines in the spectrum of alpha Sco B and mass-loss of alpha Sco A". Astronomy and Astrophysics. 70: 227. Bibcode:1978A&A....70..227K.
  12. ^ Schröder, K.-P.; Cuntz, M. (April 2007). "A critical test of empirical mass loss formulas applied to individual giants and supergiants". Astronomy and Astrophysics. 465 (2): 593–601. arXiv:astro-ph/0702172. Bibcode:2007A&A...465..593S. doi:10.1051/0004-6361:20066633.
  13. ^ a b c d e f g Allen, R.H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. pp. 364–366. ISBN 978-0-486-21079-7.
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External links

Coordinates: Sky map 16h 29m 24s, −26° 25′ 55″