Boötes
Constellation | |
13th) | |
Main stars | 7, 15 |
---|---|
Bayer/Flamsteed stars | 59 |
Stars with planets | 10 |
Stars brighter than 3.00m | 3 |
Stars within 10.00 pc (32.62 ly) | 3 |
Brightest star | Arcturus (α Boo) (−0.04m) |
Messier objects | 0 |
Meteor showers | |
Bordering constellations | |
Visible at latitudes between +90° and −50°. Best visible at 21:00 (9 p.m.) during the month of June. Other designations: Arctophylax |
Boötes (
One of the 48 constellations described by the 2nd-century astronomer
History and mythology
In
Another myth associated with Boötes by
Following another reading, the constellation is identified with Arcas and also referred to as Arcas and Arcturus, son of Zeus and Callisto. Arcas was brought up by his maternal grandfather Lycaon, to whom one day Zeus went and had a meal. To verify that the guest was really the king of the gods, Lycaon killed his grandson and prepared a meal made from his flesh. Zeus noticed and became very angry, transforming Lycaon into a wolf and giving life back to his son. In the meantime Callisto had been transformed into a she-bear by Zeus's wife Hera, who was angry at Zeus's infidelity.[8][10] This is corroborated by the Greek name for Boötes, Arctophylax, which means "Bear Watcher".[10]
Callisto, in the form of a bear was almost killed by her son, who was out hunting. Zeus rescued her, taking her into the sky where she became Ursa Major, "the Great Bear". Arcturus, the name of the constellation's brightest star, comes from the Greek word meaning "guardian of the bear". Sometimes Arcturus is depicted as leading the hunting dogs of nearby Canes Venatici and driving the bears of Ursa Major and Ursa Minor.[12]
Several
Non-Western astronomy
The stars of Boötes were incorporated into many different Chinese constellations. Arcturus was part of the most prominent of these, variously designated as the celestial king's throne (Tian Wang) or the Blue Dragon's horn (Daijiao); the name Daijiao, meaning "great horn", is more common. Arcturus was given such importance in Chinese celestial mythology because of its status marking the beginning of the lunar calendar, as well as its status as the brightest star in the northern night sky.[citation needed]
Two constellations flanked Daijiao: Yousheti to the right and Zuosheti to the left; they represented companions that orchestrated the seasons. Zuosheti was formed from modern Zeta, Omicron and Pi Boötis, while Yousheti was formed from modern Eta, Tau and Upsilon Boötis. Dixi, the Emperor's ceremonial banquet mat, was north of Arcturus, consisting of the stars 12, 11 and 9 Boötis. Another northern constellation was Qigong, the Seven Dukes, which mostly straddled the Boötes-Hercules border. It included either Delta Boötis or Beta Boötis as its terminus.[10]
The other Chinese constellations made up of the stars of Boötes existed in the modern constellation's north; they are all representations of weapons. Tianqiang, the spear, was formed from Iota, Kappa and Theta Boötis; Genghe, variously representing a lance or shield, was formed from Epsilon, Rho and Sigma Boötis.
There were also two weapons made up of a singular star. Xuange, the halberd, was represented by Lambda Boötis, and Zhaoyao, either the sword or the spear, was represented by Gamma Boötis.[10]
Two Chinese constellations have an uncertain placement in Boötes. Kangchi, the lake, was placed south of Arcturus, though its specific location is disputed. It may have been placed entirely in Boötes, on either side of the Boötes-Virgo border, or on either side of the Virgo-Libra border. The constellation Zhouding, a bronze tripod-mounted container used for food, was sometimes cited as the stars 1, 2 and 6 Boötis. However, it has also been associated with three stars in Coma Berenices.[10]
Boötes is also known to
Characteristics
Boötes is a constellation bordered by Virgo to the south, Coma Berenices and Canes Venatici to the west, Ursa Major to the northwest, Draco to the northeast, and Hercules,
Colloquially, its pattern of stars has been likened to a kite or ice cream cone.[19][20] However, depictions of Boötes have varied historically. Aratus described him circling the north pole, herding the two bears. Later ancient Greek depictions, described by Ptolemy, have him holding the reins of his hunting dogs (Canes Venatici) in his left hand, with a spear, club, or staff in his right hand.[10] After Hevelius introduced Mons Maenalus in 1681, Boötes was often depicted standing on the Peloponnese mountain.[16] By 1801, when Johann Bode published his Uranographia, Boötes had acquired a sickle, which was also held in his left hand.[10]
The placement of Arcturus has also been mutable through the centuries. Traditionally, Arcturus lay between his thighs, as Ptolemy depicted him. However,
Features
Stars
In his Uranometria, Johann Bayer used the Greek letters alpha through to omega and then A to k to label what he saw as the most prominent 35 stars in the constellation, with subsequent astronomers splitting Kappa, Mu, Nu and Pi as two stars each. Nu is also the same star as Psi Herculis.[21] John Flamsteed numbered 54 stars for the constellation.[22]
Located 36.7
Bayer located Arcturus above the Herdman's left knee in his Uranometria. Nearby
Marking the herdsman's head is Beta Boötis,
Located 86 light-years distant, Gamma Boötis, or Seginus, is a white giant star of spectral class A7III,[32] with a luminosity 34 times and diameter 3.5 times that of the Sun.[33] It is a Delta Scuti variable, ranging between magnitudes 3.02 and 3.07 every 7 hours.[34] These stars are short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study asteroseismology.[35]
Delta Boötis is a wide double star with a primary of magnitude 3.5 and a secondary of magnitude 7.8. The primary is a yellow giant that has cooled and expanded to 10.4 times the diameter of the Sun.[36] Of spectral class G8IV, it is around 121 light-years away,[37] while the secondary is a yellow main sequence star of spectral type G0V.[38] The two are thought to take 120,000 years to orbit each other.[36]
Nu Boötis is an optical double star. The primary is an orange giant of magnitude 5.0 and the secondary is a white star of magnitude 5.0. The primary is 870 light-years away and the secondary is 430 light-years.
Nearby Rho and Sigma Boötis denote the herdsman's waist.[26] Rho is an orange giant of spectral type K3III located around 160 light-years from Earth.[41] It is ever so slightly variable, wavering by 0.003 of a magnitude from its average of 3.57.[42] Sigma, a yellow-white main-sequence star of spectral type F3V, is suspected of varying in brightness from 4.45 to 4.49.[42] It is around 52 light-years distant.[43]
Traditionally known as Aulād al Dhiʼbah (أولاد الضباع – aulād al dhiʼb), "the Whelps of the Hyenas", Theta, Iota, Kappa and Lambda Boötis (or Xuange[44]) are a small group of stars in the far north of the constellation. The magnitude 4.05 Theta Boötis has a spectral type of F7 and an absolute magnitude of 3.8. Iota Boötis is a triple star with a primary of magnitude 4.8 and spectral class of A7,[13] a secondary of magnitude 7.5,[8] and a tertiary of magnitude 12.6.[40] The primary is 97 light-years away.[8] The primary and secondary stars are separated by 38.5 arcseconds, at an angle of 33 degrees.[13] The primary and tertiary stars are separated by 86.7 arcseconds at an angle of 194 degrees. Both the primary and tertiary appear white in a telescope, but the secondary appears yellow-hued.[40]
Kappa Boötis is another wide double star. The primary is 155 light-years away and has a magnitude of 4.5. The secondary is 196 light-years away and has a magnitude of 6.6.[8] The two components are separated by 13.4 arcseconds, at an angle of 236 degrees.[13] The primary, with spectral class A7, appears white and the secondary appears bluish.[40]
An apparent magnitude 4.18 type A0p star,[13] Lambda Boötis is the prototype of a class of chemically peculiar stars, only some of which pulsate as Delta Scuti-type stars. The distinction between the Lambda Boötis stars as a class of stars with peculiar spectra, and the Delta Scuti stars whose class describes pulsation in low-overtone pressure modes, is an important one. While many Lambda Boötis stars pulsate and are Delta Scuti stars, not many Delta Scuti stars have Lambda Boötis peculiarities, since the Lambda Boötis stars are a much rarer class whose members can be found both inside and outside the Delta Scuti instability strip. Lambda Boötis stars are dwarf stars that can be either spectral class A or F.[45] Like BL Boötis-type stars they are metal-poor.[46] Scientists have had difficulty explaining the characteristics of Lambda Boötis stars, partly because only around 60 confirmed members exist, but also due to heterogeneity in the literature. Lambda has an absolute magnitude of 1.8.[13]
There are two dimmer F-type stars, magnitude 4.83 12 Boötis, class F8; and magnitude 4.93 45 Boötis, class F5.[13] Xi Boötis is a G8 yellow dwarf of magnitude 4.55, and absolute magnitude is 5.5. Two dimmer G-type stars are magnitude 4.86 31 Boötis, class G8, and magnitude 4.76 44 Boötis, class G0.[13]
Of apparent magnitude 4.06,
There is one bright B-class star in Boötes; magnitude 4.93
Multiple stars
Besides Pulcherrima and Alkalurops, there are several other binary stars in Boötes:
- Xi Boötis is a quadruple star popular with amateur astronomers. The primary is a yellow star of magnitude 4.7 and the secondary is an orange star of magnitude 6.8. The system is 22 light-years away and has an orbital period of 150 years.[8] The primary and secondary have a separation of 6.7 arcseconds at an angle of 319 degrees.[13] The tertiary is a magnitude 12.6 star (though it may be observed to be brighter) and the quaternary is a magnitude 13.6 star.[40]
- Pi Boötis is a close triple star. The primary is a blue-white star of magnitude 4.9, the secondary is a blue-white star of magnitude 5.8,[8] and the tertiary is a star of magnitude 10.4.[40] The primary and secondary components are separated by 5.6 arcseconds at an angle of 108 degrees;[13] the primary and tertiary components are separated by 128 arcseconds at an angle of 128 degrees.[40]
- Zeta Boötis is a triple star that consists of a physical binary pair with an optical companion. Lying 205 light-years away from Earth, The physical pair has a period of 123.3 years and consists of a magnitude 4.5 and a magnitude 4.6 star. The two components are separated by 1.0 arcseconds at an angle of 303 degrees. The optical companion is of magnitude 10.9, separated by 99.3 arcseconds at an angle of 259 degrees. 44 Boötis is an eclipsing variable star. The primary is of variable magnitude and the secondary is of magnitude 6.2; they have an orbital period of 225 years. The components are separated by 1.0 arcsecond at an angle of 40 degrees.[13]
44 Boötis (i Boötis) is a double variable star 42 light-years away. It has an overall magnitude of 4.8 and appears yellow to the naked eye. The primary is of magnitude 5.3 and the secondary is of magnitude 6.1; their orbital period is 220 years. The secondary is itself an eclipsing variable star with a range of 0.6 magnitudes; its orbital period is 6.4 hours.[8] It is a W Ursae Majoris variable that ranges in magnitude from a minimum of 7.1 to a maximum of 6.5 every 0.27 days. Both stars are G-type stars. Another eclipsing binary star is ZZ Boötis, which has two F2-type components of almost equal mass,[47] and ranges in magnitude from a minimum of 6.79 to a maximum of 7.44 over a period of 5.0 days.[48]
Variable stars
Two of the brighter Mira-type variable stars in the constellation are
BL Boötis is the prototype of its class of pulsating variable stars,[50] the anomalous Cepheids. These stars are somewhat similar to Cepheid variables, but they do not have the same relationship between their period and luminosity.[51] Their periods are similar to RRAB variables; however, they are far brighter than these stars.[52] BL Boötis is a member of the cluster NGC 5466. Anomalous Cepheids are metal poor and have masses not much larger than the Sun's, on average, 1.5 M☉. BL Boötis type stars are a subtype of RR Lyrae variables.[53]
Stars with planetary systems
Like Tau Boötis b, HAT-P-4b is also a hot Jupiter. It is noted for orbiting a particularly metal-rich host star and being of low density.[58] Discovered in 2007, HAT-P-4 b has a mass of 0.68 MJ and a radius of 1.27 RJ. It orbits every 3.05 days at a distance of 0.04 AU. HAT-P-4, the host star, is an F-type star of magnitude 11.2, 310 parsecs from Earth. It is larger than the Sun, with a mass of 1.26 M☉ and a radius of 1.59 R☉.[59]
Boötes is also home to multiple-planet systems. HD 128311 is the host star for a two-planet system, consisting of HD 128311 b and HD 128311 c, discovered in 2002 and 2005, respectively.[60][61] HD 128311 b is the smaller planet, with a mass of 2.18 MJ; it was discovered through radial velocity observations. It orbits at almost the same distance as Earth, at 1.099 AU; however, its orbital period is significantly longer at 448.6 days.[60]
The larger of the two, HD 128311 c, has a mass of 3.21 MJ and was discovered in the same manner. It orbits every 919 days inclined at 50°, and is 1.76 AU from the host star.[61] The host star, HD 128311, is a K0V-type star located 16.6 parsecs from Earth. It is smaller than the Sun, with a mass of 0.84 M☉ and a radius of 0.73 R☉; it also appears below the threshold of naked-eye visibility at an apparent magnitude of 7.51.[60]
There are several single-planet systems in Boötes. HD 132406 is a Sun-like star of spectral type G0V with an apparent magnitude of 8.45, 231.5 light-years from Earth.[62] It has a mass of 1.09 M☉ and a radius of 1 R☉.[63] The star is orbited by a gas giant, HD 132406 b, discovered in 2007.[62] HD 132406 orbits 1.98 AU from its host star with a period of 974 days and has a mass of 5.61 MJ. The planet was discovered by the radial velocity method.[63]
Another single planetary system in Boötes is the
Also discovered through the radial velocity method, albeit a year earlier, is
Deep-sky objects
Boötes is in a part of the
Boötes has two bright galaxies.
Further away lies the 250-million-light-year-diameter
The Hercules–Corona Borealis Great Wall, the largest-known structure in the Universe, covers a significant part of Boötes.[82]
Meteor showers
Boötes is home to the
The Quadrantids are notoriously difficult to observe because of a low radiant and often inclement weather. The parent body of the meteor shower has been disputed for decades;[83] however, Peter Jenniskens has proposed 2003 EH1, a minor planet, as the parent.[85] 2003 EH1 may be linked to C/1490 Y1, a comet previously thought to be a potential parent body for the Quadrantids.[86][87]
2003 EH1 is a
On April 28, 1984, a remarkable outburst of the normally placid Alpha Bootids was observed by visual observer Frank Witte from 00:00 to 2:30 UTC. In a 6 cm telescope, he observed 433 meteors in a field of view near Arcturus with a diameter of less than 1°. Peter Jenniskens comments that this outburst resembled a "typical dust trail crossing".[91] The Alpha Bootids normally begin on April 14, peaking on April 27 and 28, and finishing on May 12.[92] Its meteors are slow-moving, with a velocity of 20.9 kilometers per second.[93] They may be related to Comet 73P/Schwassmann–Wachmann 3, but this connection is only theorized.[92]
The June Bootids, also known as the Iota Draconids, is a meteor shower associated with the comet 7P/Pons–Winnecke, first recognized on May 27, 1916, by William F. Denning.[94] The shower, with its slow meteors, was not observed prior to 1916 because Earth did not cross the comet's dust trail until Jupiter perturbed Pons–Winnecke's orbit, causing it to come within 0.03 AU (4.5 million km; 2.8 million mi) of Earth's orbit the first year the June Bootids were observed.
In 1982, E. A. Reznikov discovered that the 1916 outburst was caused by material released from the comet in 1819.[95] Another outburst of the June Bootids was not observed until 1998, because Comet Pons–Winnecke's orbit was not in a favorable position. However, on June 27, 1998, an outburst of meteors radiating from Boötes, later confirmed to be associated with Pons-Winnecke, was observed. They were incredibly long-lived, with trails of the brightest meteors lasting several seconds at times. Many fireballs, green-hued trails, and even some meteors that cast shadows were observed throughout the outburst, which had a maximum zenithal hourly rate of 200–300 meteors per hour.[96]
Two Russian astronomers determined in 2002 that material ejected from the comet in 1825 was responsible for the 1998 outburst.[97] Ejecta from the comet dating to 1819, 1825 and 1830 was predicted to enter Earth's atmosphere on June 23, 2004. The predictions of a shower less spectacular than the 1998 showing were borne out in a display that had a maximum zenithal hourly rate of 16–20 meteors per hour that night. The June Bootids are not expected to have another outburst in the next 50 years.[98]
Typically, only 1–2 dim, very slow meteors are visible per hour; the average June Bootid has a magnitude of 5.0. It is related to the Alpha Draconids and the Bootids-Draconids. The shower lasts from June 27 to July 5, with a peak on the night of June 28.[99] The June Bootids are classified as a class III shower (variable),[100] and has an average entry velocity of 18 kilometers per second. Its radiant is located 7 degrees north of Beta Boötis.[101]
The Beta Bootids is a weak shower that begins on January 5, peaks on January 16, and ends on January 18. Its meteors travel at 43 km/s.[102] The January Bootids is a short, young meteor shower that begins on January 9, peaks from January 16 to January 18, and ends on January 18.[103]
The Phi Bootids is another weak shower radiating from Boötes. It begins on April 16, peaks on April 30 and May 1, and ends on May 12.[92] Its meteors are slow-moving, with a velocity of 15.1 km/s. They were discovered in 2006.[104] The shower's peak hourly rate can be as high as six meteors per hour. Though named for a star in Boötes, the Phi Bootid radiant has moved into Hercules.[105] The meteor stream is associated with three different asteroids: 1620 Geographos, 2062 Aten and 1978 CA.[106]
The
There are several minor showers in Boötes, some of whose existence is yet to be verified. The Rho Bootids radiate from near the namesake star, and were hypothesized in 2010.[110] The average Rho Bootid has an entry velocity of 43 km/s.[110][111] It peaks in November and lasts for three days.
The Rho Bootid shower is part of the
See also
References
Citations
- ^ a b c Thompson & Thompson 2007, p. 102.
- ^ a b c IAU, The Constellations, Boötes.
- ^ White 2008, p. 207.
- Bibcode:2014SPP...253....1B. Archived(PDF) from the original on 2022-10-09.
- ^ Homer, Odyssey, book 5, 272
- ^ Mandelbaum 1990, p. 103.
- ^ Levy 1996 pp=141
- ^ a b c d e f g h i j k l m n o Ridpath 2001, pp. 88–89.
- ^ Levy 1996 pp=141
- ^ a b c d e f g h i j Star Tales Boötes.
- ^ Pasachoff 2000, p. 133.
- ^ Levy 1996 pp=141
- ^ a b c d e f g h i j k l m n o p q r s t u v w x y Moore 2000, pp. 341–342.
- ^ Levy 2008, p. 51.
- ^ Star Tales Quadrans Muralis.
- ^ a b Star Tales Mons Maenalus.
- ^ Jacobson 2012.
- ^ Russell 1922, p. 469.
- ^ a b Bakich 1995, p. 150.
- ^ Polakis 2009.
- ^ Wagman 2003, pp. 55–57.
- ^ Wagman 2003, p. 355–56.
- ^ a b SIMBAD Alpha Boötis.
- ^ a b c Moore & Tirion 1997, pp. 132–133.
- ^ Kaler Arcturus.
- ^ a b c Wagman 2003, p. 503.
- ^ SIMBAD Eta Boötis.
- ^ Kaler Muphrid.
- ^ Schaaf 2008, p. 136.
- ^ SIMBAD Beta Boötis.
- ^ Kaler Nekkar.
- ^ SIMBAD Gamma Boötis.
- ^ Kaler Seginus.
- ^ AAVSO Gamma Boötis.
- ^ AAVSO Delta Scuti Variables.
- ^ a b Kaler Delta Boötis.
- ^ SIMBAD Delta Boötis.
- ^ SIMBAD BD+33 2562.
- ^ Thompson & Thompson 2007, p. 106.
- ^ a b c d e f g h i Thompson & Thompson 2007, p. 105.
- ^ SIMBAD Rho Boötis.
- ^ a b AAVSO Rho Boötis.
- ^ SIMBAD Sigma Boötis.
- ^ "Naming Stars". IAU.org. Retrieved 30 July 2018.
- ^ North 2004, p. 145.
- ^ Good 2003, p. 62.
- ^ Popper 1983.
- ^ AAVSO ZZ Boötis.
- ^ Pasachoff 2000, pp. 199–200.
- ^ North 2004, p. 123.
- ^ Good 2003, p. 61.
- ^ Good 2003, p. 69.
- ^ Good 2003, p. 70.
- ^ Exoplanet Encyclopedia Tau Boo b.
- ^ a b Rodler, Lopez-Morales & Ribas 2012.
- ^ Cameron et al. 2000.
- ^ a b Walker et al. 2008.
- ^ Kovács et al. 2007.
- ^ Exoplanet Encyclopedia HAT-P-4 b.
- ^ a b c Exoplanet Encyclopedia HD 128311 b.
- ^ a b Exoplanet Encyclopedia HD 128311 c.
- ^ a b Da Silva Udry et al. 2007.
- ^ a b Exoplanet Encyclopedia HD 132406.
- ^ Exoplanet Encyclopedia WASP-23 b.
- ^ Exoplanet Encyclopedia HD 131496 b.
- ^ Exoplanet Encyclopedia HD 132563B b.
- ^ Desidera et al. 2011.
- ^ Exoplanet Encyclopedia HD 136418 b.
- ^ a b c Joshi et al. 2009.
- ^ a b Exoplanet Encyclopedia WASP-14 b.
- ^ Thompson & Thompson 2007, p. 103.
- ^ Thompson & Thompson 2007, p. 104.
- ^ Niksch & Block 2004.
- ^ SIMBAD NGC 5008.
- ^ SIMBAD NGC 5548.
- ^ SIMBAD NGC 5653.
- ^ SIMBAD NGC 5825.
- ^ SIMBAD NGC 5778.
- ^ SIMBAD NGC 5886.
- ^ SIMBAD NGC 5888.
- ^ Francis, Matthew R. "What's 250 Million Light-Years Big, Almost Empty, and Full of Answers?". Nautilus. Archived from the original on 2018-07-17. Retrieved 2018-07-17.
- S2CID 56073380. Retrieved 2018-06-19.
- ^ a b Jenniskens 2006, pp. 357–368.
- ^ Jenniskens 2006, p. 612.
- ^ Jenniskens 2006, p. 368.
- ^ Jenniskens 2006, p. 373.
- ^ Jenniskens 2006, p. 376.
- ^ a b Jenniskens 2012.
- ^ Levy 2008, p. 49.
- ^ Levy 2008, p. 104.
- ^ Jenniskens 2006, p. 199.
- ^ a b c Levy 2008, p. 110.
- ^ IAU Alpha Bootids.
- ^ Jenniskens 2006, p. 334.
- ^ Jenniskens 2006, p. 335.
- ^ Jenniskens 2006, p. 336–337.
- ^ Jenniskens 2006, p. 338.
- ^ Jenniskens 2006, p. 339–344.
- ^ Levy 2008, p. 113.
- ^ AMS 2012 List.
- ^ AMS June 23.
- ^ Levy 2008, p. 105.
- ^ Levy 2008, p. 106.
- ^ IAU Phi Bootids.
- ^ Koed & Sherrod 2003, p. 52.
- ^ Štohl & Porubčan 1993, p. 43.
- ^ IAU Lambda Bootids.
- ^ IAU Bootid-Coronae Borealid Complex.
- ^ Green 2007.
- ^ a b IAU Rho Bootids.
- ^ a b Brown et al. 2010.
- ^ IAU Gamma Bootids.
- ^ IAU Nu Bootids.
References
- Templeton, Matthew (16 July 2010). "Delta Scuti and the Delta Scuti Variables". Variable Star of the Season. AAVSO (American Association of Variable Star Observers). Retrieved 3 November 2012.
- Watson, Christopher (4 January 2010). "Gamma Boötis". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 August 2014.
- Watson, Christopher (3 May 2013). "NSV 6697". AAVSO Website. American Association of Variable Star Observers. Retrieved 8 August 2014.
- Watson, Christopher (18 January 2010). "NSV 6717". AAVSO Website. American Association of Variable Star Observers. Retrieved 8 August 2014.
- Watson, Christopher (4 January 2010). "ZZ Boötis". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 August 2014.
- da Silva, Ronaldo; Udry, Stéphane; Bouchy, François; Moutou, Claire; Mayor, Michel; Beuzit, Jean-Luc; Bonfils, Xavier; Delfosse, Xavier; Desort, Morgan; Forveille, Thierry; Galland, Franck; Hébrard, Guillaume; Lagrange, Anne-Marie; Loeillet, Benoit; Lovis, Christophe; Pepe, Francesco; Perrier, Christian; Pont, Frédéric; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Sivan, Jean-Pierre; Vidal-Madjar, Alfred; Zucker, Shay (October 2007). "ELODIE metallicity-biased search for transiting Hot Jupiters IV. Intermediate period planets orbiting the stars HD 43691 and HD 132406". S2CID 18805775. (web preprint)
- Bakich, Michael E. (1995). The Cambridge Guide to the Constellations. Cambridge University Press. ISBN 978-0-521-44921-2.
- Brown, P.; Wong, D.K.; Weryk, R.J.; Wiegert, P. (May 2010). "A meteoroid stream survey using the Canadian Meteor Orbit Radar: II: Identification of minor showers using a 3D wavelet transform". Icarus. 207 (1): 66–81. .
- Collier Cameron, Andrew; Horne, Keith; James, David; Penny, Alan; Semel, Meir (8 December 2000). "τ Boo b: Not so bright, but just as heavy". Planetary Systems in the Universe: Observation, Formation, and Evolution.
- Desidera, S.; Carolo, E.; Gratton, R.; Martinez Fiorenzano, A.F.; Endl, M.; Mesa, D.; Barbieri, M.; Bonavita, M.; Cecconi, M.; Claudi, R.U.; Cosentino, R.; Marzari, F.; Scuderi, S. (7 September 2011). "A giant planet in the triple system HD 132563". Astronomy & Astrophysics. 533. Claudi, R. U.; Cosentino, R.; Marzari, F.; and Scuderi, S.: A90. S2CID 54938087.
- "Tau Boo b". Extrasolar Planets Encyclopaedia. 5 July 2012. Archived from the original on 1 December 2019. Retrieved 31 August 2012.
- "HD 128311 b". Extrasolar Planets Encyclopaedia. 4 January 2011. Retrieved 4 September 2012.
- "HD 128311 c". Extrasolar Planets Encyclopaedia. 11 May 2011. Retrieved 4 September 2012.
- "WASP-23 b". Extrasolar Planets Encyclopaedia. 24 March 2011. Retrieved 4 September 2012.
- "HD 131496 b". Extrasolar Planets Encyclopaedia. 2 September 2011. Retrieved 4 September 2012.
- "HD 132406 b". Extrasolar Planets Encyclopaedia. 31 October 2007. Retrieved 5 September 2012.
- "HD 132563B b". Extrasolar Planets Encyclopaedia. 6 July 2011. Archived from the original on 13 October 2014. Retrieved 5 September 2012.
- "HD 136418 b". Extrasolar Planets Encyclopaedia. 19 March 2010. Retrieved 5 September 2012.
- "HAT-P-4 b". Extrasolar Planets Encyclopaedia. 5 April 2012. Retrieved 5 September 2012.
- "WASP-14 b". Extrasolar Planets Encyclopaedia. 8 April 2012. Retrieved 5 September 2012.
- Good, Gerry A. (2003). Observing Variable Stars. Springer. ISBN 978-1-85233-498-7.
- Green, Daniel W. E. (17 November 2007). "Thirteen New Meteor Showers Recognized". Electronic Telegram No. 1142. Central Bureau for Astronomical Telegrams, IAU. Retrieved 9 September 2012.
- "Alpha Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Bootid-Coronae Borealid Complex". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Gamma Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Lambda Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Nu Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Phi Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 9 September 2012.
- "Rho Bootids". Meteor Shower Center. IAU. 5 September 2012. Retrieved 7 September 2012.
- Jacobson, Steven A. (2012). Yup'ik Eskimo Dictionary, 2nd edition. Alaska Native Language Center. ISBN 9781555001155.
- Jenniskens, Peter (2006). Meteor Showers and their Parent Comets. Cambridge University Press. ISBN 978-0-521-85349-1.
- Jenniskens, Peter (September 2012). "Mapping Meteoroid Orbits: New Meteor Showers Discovered". Sky & Telescope: 24.
- Joshi, Y. C.; Pollacco, D.; Collier Cameron, A.; Skillen, I.; Simpson, E.; Steele, I.; Street, R. A.; Stempels, H. C.; et al. (February 2009). "WASP-14b: 7.3 MJ transiting planet in an eccentric orbit". S2CID 7775011.
- Kaler, Jim. "Arcturus". Stars. University of Illinois. Retrieved 6 August 2014.
- Kaler, Jim. "Delta Boötis". Stars. University of Illinois. Retrieved 10 August 2014.
- Kaler, Jim. "Muphrid". Stars. University of Illinois. Retrieved 7 August 2014.
- Kaler, Jim. "Nekkar". Stars. University of Illinois. Retrieved 6 August 2014.
- Kaler, Jim. "Seginus". Stars. University of Illinois. Retrieved 8 August 2014.
- Koed, Thomas L.; Sherrod, P. Clay (2003). A Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations. Courier Dover Publications. ISBN 9780486428208.
- Kovács, G.; Bakos, G. Á.; Torres, G.; Sozzetti, A.; Latham, D. W.; Noyes, R. W.; Butler, R. P.; Marcy, G. W.; Fischer, D. A.; Fernández, J. M.; Esquerdo, G.; Sasselov, D. D.; Stefanik, R. P.; Pál, A.; Lázár, J.; Papp, I.; Sári, P. (20 November 2007). "HAT-P-4b: A Metal-rich Low-Density Transiting Hot Jupiter". The Astrophysical Journal. 670 (1). Fernández, J. M.; Esquerdo, G.; Sasselov, D. D.; Stefanik, R. P.; Pál, A.; Lázár, J.; Papp, I.; Sári, P.: L41. S2CID 14966730.
- Levy, David H. (2008). David Levy's Guide to Observing Meteor Showers. Cambridge University Press. ISBN 978-0-521-69691-3.
- Lunsford, Robert (16 January 2012). "2012 Meteor Shower List". American Meteor Society. Retrieved 7 September 2012.
- Lunsford, Robert (21 June 2012). "Meteor Activity Outlook for June 23-29 2012". American Meteor Society. Retrieved 7 September 2012.
- Moore, Patrick; Tirion, Wil (1997). Cambridge Guide to Stars and Planets (2nd ed.). Cambridge University Press. ISBN 978-0-521-58582-8.
- Mandelbaum, Allen; translator (1990). The Odyssey of Homer. New York City: Bantam Dell. ISBN 978-0-553-21399-7.)
{{cite book}}
:|first=
has generic name (help)CS1 maint: multiple names: authors list (link - Moore, Patrick (2000). The Data Book of Astronomy. Institute of Physics Publishing. ISBN 978-0-7503-0620-1.
- North, Gerald (2004). Observing Variable Stars, Novae, and Supernovae. Cambridge University Press. ISBN 978-0-521-82047-9.
- Niksch, Dale; Block, Adam (16 May 2004). "Best of AOP: NGC 5248". NOAO. Archived from the original on 13 October 2014. Retrieved 1 September 2012.
- Pasachoff, Jay M. (2000). Stars and Planets (4th ed.). Houghton Mifflin. ISBN 978-0-395-93431-9.
- Polakis, Tom (3 March 2009). "Boötes and Corona Borealis". Astronomy Magazine. Retrieved 13 August 2012.
- Popper, D. M. (1983). "The F-type eclipsing binaries ZZ Bootis, CW Eridani, and BK Pegasi". Astronomical Journal. 88: 1242–56. ISSN 0004-6256.
- Ridpath, Ian (2001). Stars and Planets Guide. Princeton University Press. ISBN 978-0-691-08913-3.
- Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide (4th ed.). Princeton University Press. ISBN 978-0-691-13556-4.
- Ridpath, Ian. "Boötes". Star Tales. Retrieved 10 September 2012.
- Ridpath, Ian. "Mons Maenalus". Star Tales. Retrieved 21 September 2012.
- Ridpath, Ian. "Quadrans Muralis". Star Tales. Retrieved 21 September 2012.
- Rodler, F.; Lopez-Morales, M.; Ribas, I. (18 June 2012). "Weighing the non-transiting hot Jupiter τ Boo b". The Astrophysical Journal Letters. 753 (1): L25. S2CID 119177983.
- Russell, Henry Norris (October 1922). "The new international symbols for the constellations". Popular Astronomy. 30: 469. Bibcode:1922PA.....30..469R.
- Schilling, Govert (2011). Atlas of Astronomical Discoveries. New York, New York: Springer Science & Business Media. ISBN 9781441978110.
- Schaaf, Fred (2008). The Brightest Stars: Discovering the Universe Through the Sky's Most Brilliant Stars. Hoboken, New Jersey: John Wiley and Sons. ISBN 978-0-471-70410-2.
- "Alpha Boötis - Red Giant Branch Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 6 August 2014.
- "Eta Boötis - Spectroscopic Binary". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 7 August 2014.
- "Beta Boötis - Flare Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 6 August 2014.
- "Delta Boötis - Star in double system". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 10 August 2014.
- "BD+33 2562 - High proper motion star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 10 August 2014.
- "Gamma Boötis - Variable star of Delta Scuti type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 8 August 2014.
- "Rho Boötis - Variable star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 8 August 2014.
- "Sigma Boötis - Variable star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 8 August 2014.
- "NGC 5008". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5548". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5778". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5653". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5825". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5886". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- "NGC 5888". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 August 2012.
- Štohl, J.; Porubčan, V. (6 July 1993). "Meteor streams of asteroidal origin". Meteoroids and Their Parent Bodies, Proceedings of the International Astronomical Symposium: 41. Bibcode:1993mtpb.conf...41S.
- Thompson, Robert Bruce; Thompson, Barbara Fritchman (2007). Illustrated Guide to Astronomical Wonders. O'Reilly Books. ISBN 978-0-596-52685-6.
- Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, ISBN 978-0-939923-78-6.
- White, Gavin (2008). Babylonian Star-lore. Solaria Publications.
- Walker, G. A. H.; Croll, B.; Matthews, J. M.; Kuschnig, R.; Huber, D.; Weiss, W. W.; Shkolnik, E.; Rucinski, S. M.; Guenther, D. B. (19 February 2008). "MOST detects variability on τ Bootis A possibly induced by its planetary companion". Astronomy & Astrophysics. 482 (2). Moffat, A. F. J.; Sasselov, D.: 691–697. S2CID 56317105. Retrieved 31 August 2012.
- "Boötes, constellation boundary". The Constellations. International Astronomical Union. Retrieved 3 July 2012.