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An orange giant of spectral class K1. Bayer located Arcturus above the Herdman's left knee in his Uranometria. Nearby Eta Boötis , or Muphrid, is the uppermost star denoting the left leg.

It is 9 times as luminous as the Sun and has 2. Analysis of its spectrum reveals that it is a spectroscopic binary. Marking the herdsman's head is Beta Boötis, [26] or Nekkar, a yellow giant of magnitude 3.

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.

Delta Boötis is a wide double star with a primary of magnitude 3. The primary is a yellow giant that has cooled and expanded to Mu Boötis , known as Alkalurops , is a triple star popular with amateur astronomers.

It has an overall magnitude of 4. Its name is from the Arabic phrase for "club" or "staff". The primary appears to be of magnitude 4.

The secondary appears to be of magnitude 6. The secondary and tertiary stars have an orbital period of years. Nu Boötis is an optical double star.

The primary is an orange giant of magnitude 5. The primary is light-years away and the secondary is light-years. Epsilon Boötis , also known as Izar or Pulcherrima , is a close triple star popular with amateur astronomers and the most prominent binary star in Boötes.

The primary is a yellow- [40] or orange-hued magnitude 2. The name "Izar" comes from the Arabic word for "girdle" or "loincloth", referring to its location in the constellation.

The name "Pulcherrima" comes from the Latin phrase for "most beautiful", referring to its contrasting colors in a telescope.

Nearby Rho and Sigma Boötis denote the herdsman's waist. The magnitude 4. Iota Boötis is a triple star with a primary of magnitude 4.

Both the primary and tertiary appear white in a telescope, but the secondary appears yellow-hued.

Kappa Boötis is another wide double star. The primary is light-years away and has a magnitude of 4. The secondary is light-years away and has a magnitude of 6.

An apparent magnitude 4. 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. Lambda has an absolute magnitude of 1. There are two dimmer F-type stars , magnitude 4.

Two dimmer G-type stars are magnitude 4. Of apparent magnitude 4. Dimmer than Upsilon Boötis is magnitude 4. Just slightly dimmer than Phi at magnitude 4.

O Boötis has an absolute magnitude of 0. The other four dim stars are magnitude 4. There is one bright B-class star in Boötes; magnitude 4.

It has a spectral class of B9 and is 40 parsecs from Earth. There is also one M-type star, magnitude 4. It is of class gM0. The primary is of magnitude 5.

The secondary is itself an eclipsing variable star with a range of 0. 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.

Two of the brighter Mira-type variable stars in the constellation are R and S Boötis. Both are red giants that range greatly in magnitude—from 6.

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.

Anomalous Cepheids are metal poor and have masses not much larger than the Sun's, on average, 1. T Boötis was a nova observed in April at a magnitude of 9.

It has never been observed since, but that does not preclude the possibility of it being a highly irregular variable star or a recurrent nova.

Extrasolar planets have been discovered encircling ten stars in Boötes as of Tau Boötis is orbited by a large planet, discovered in The host star itself is a magnitude 4.

It has a mass of 1. Tau Boötis b , the sole planet discovered in the system, orbits at a distance of 0.

Discovered through radial velocity measurements, it has a mass of 5. Furthermore, a slight variability in the host star's light may be caused by magnetic interactions with the planet.

Tau Boötis b does not transit its star, rather, its orbit is inclined 46 degrees. It is noted for orbiting a particularly metal-rich host star and being of low density.

It orbits every 3. HAT-P-4 , the host star, is an F-type star of magnitude It is larger than the Sun, with a mass of 1.

Boötes is also home to multiple-planet systems. HD is the host star for a two-planet system, consisting of HD b and HD c , discovered in and , respectively.

It orbits at almost the same distance as Earth, at 1. The larger of the two, HD c, has a mass of 3. It is smaller than the Sun, with a mass of 0.

There are several single-planet systems in Boötes. HD is a Sun-like star of spectral type G0V with an apparent magnitude of 8. The planet was discovered by the radial velocity method.

The planet, discovered by the transit method in , orbits every 2. It is smaller than Jupiter, at 0. Its star is a K1V type star of apparent magnitude HD is also encircled by one planet, HD b.

The star is of type K0 and is located parsecs from Earth; it appears at a visual magnitude of 7. It is significantly larger than the Sun, with a mass of 1.

Its one planet, discovered in by the radial velocity method , has a mass of 2. HD b orbits at a distance of 2. Another single planetary system in Boötes is the HD system, a triple star system.

The parent star, technically HD B , is a star of magnitude 9. Its planet, HD B b , was discovered in by the radial velocity method. HD B b is one of very few planets found in triple star systems; it orbits the isolated member of the system, which is separated from the other components, a spectroscopic binary , by AU.

Also discovered through the radial velocity method, albeit a year earlier, is HD b , a 2-Jupiter mass planet that orbits the star HD at a distance of 1.

Its host star is a magnitude 7. It has a radius of 3. WASP b is one of the most massive and dense exoplanets known, [69] with a mass of 7.

Discovered via the transit method, it orbits 0. It has a radius of 1. Boötes is in a part of the celestial sphere facing away from the plane of our home Milky Way galaxy, and so does not have open clusters or nebulae.

Instead, it has one bright globular cluster and many faint galaxies. Only approximately 12 stars are resolved by an amateur instrument.

Boötes has two bright galaxies. NGC Caldwell 45 is a type Sc galaxy a variety of spiral galaxy of magnitude It measures 6.

It measures 3. Further away lies the million-light-year-diameter Boötes void , a huge space largely empty of galaxies. Discovered by Robert Kirshner and colleagues in , it is roughly million light-years from Earth.

Boötes is home to the Quadrantid meteor shower, the most prolific annual meteor shower. It was discovered in January and named in by Alexander Hershell.

Quadrantid meteors are dim, but have a peak visible hourly rate of approximately per hour on January 3—4. 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 EH 1 , a minor planet, as the parent.

It is now dormant. Peter Jenniskens comments that this outburst resembled a "typical dust trail crossing". In , E. Reznikov discovered that the outburst was caused by material released from the comet in However, on June 27, , 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 — meteors per hour.

Two Russian astronomers determined in that material ejected from the comet in was responsible for the outburst.

The predictions of a shower less spectacular than the 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. Typically, only 1—2 dim, very slow meteors are visible per hour; the average June Bootid has a magnitude of 5.

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 Its radiant is located 7 degrees north of Beta Boötis.

The Beta Bootids is a weak shower that begins on January 5, peaks on January 16, and ends on January 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 They were discovered in Though named for a star in Boötes, the Phi Bootid radiant has moved into Hercules.

The Lambda Bootids , part of the Bootid-Coronae Borealid Complex , are a weak annual shower with moderately fast meteors; 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 However, the link to the Taurid shower remains unconfirmed and may be a chance correlation.

Gamma Bootids have an entry velocity of From Wikipedia, the free encyclopedia. Constellation in the northern celestial hemisphere. This article is about the Northern constellation.

List of stars in Boötes. January Bootids June Bootids Quadrantids. See also: List of stars in Boötes. Sino-Platonic Papers. Bibcode : SPP Retrieved 30 July Retrieved Templeton, Matthew 16 July Variable Star of the Season.

Retrieved 3 November Watson, Christopher 4 January American Association of Variable Star Observers. Retrieved 5 August Watson, Christopher 3 May Retrieved 8 August Watson, Christopher 18 January Da Silva, R.

October Intermediate period planets orbiting the stars HD and HD ". Astronomy and Astrophysics. The Cambridge Guide to the Constellations.

Cambridge University Press. May Bibcode : Icar.. Desidera, S. Claudi, R. The Extrasolar Planets Encyclopedia. Paris Observatory.

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