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Beta Painter

Beta Painter (β Pic, β Pictoris) is the second brightest star in the constellation of the Painter . It is located at a distance of 63.4 light years from the solar system , 1.75 times more massive than the Sun and has 8.7 times more luminosity than the last. The Beta Painter’s system is very young, about 8–20 million years old [8] , although it is already at the evolutionary stage of the main sequence star [6] . Beta Painter is part of the so-called moving group of stars Beta Painter is an association of young stars moving in the same direction and having approximately the same age [8] .

β Painter
Star
Pictor constellation map.svg
Observational data
( Age J2000.0)
Right ascension
Declination
Distance63.4 ± 0.1 St. years (19.3 ± 0.05 pc )
Visible magnitude ( V )3,861 [1]
ConstellationPainter
Astrometry
Radial velocity ( R v )+20.0 ± 0.7 [2] km / s
Own movement (μ)RA: +4.65 [3]
Dec: +83,10 [3]
Parallax (π)51.44 ± 0.12 mas
Absolute magnitude (V)2.42 [note 1]
Specifications
Spectral classA6V [4]
Color Index ( B - V )0.17 [5]
Color Index ( U - B )0.10 [5]
VariabilityShield Deltas
physical characteristics
Weight1.75 [6] M ☉
Radius1.8 [7] R ☉
Age12 +8
−4 million [8] years
Temperature8052 [4] K
Luminosity8.7 [6] L ☉
Metallicity112% of the sun [4] [note 2]
Rotation130 km / s [9]
Other designations
GJ 219, HR 2020, CD −51 ° 1620, HD 39060, GCTP 1339.00, SAO 234134, HIP 27321
Database Information
SIMBAD

Compared to ordinary stars of its type, Beta Painter has an excess of infrared radiation , which, apparently, is caused by an abundance of dust near the star. Careful observations revealed a large disk of gas and dust in the star, which was the first fragmentation disk photographed near the star [10] . In addition to several belts from planetesimals [11] and comets [12] , there are signs that planets have appeared inside the disk and that the process of planet formation may still be in progress [13] . It is believed that the main source of interstellar meteoroids in our solar system is precisely the fragmentation disk near the Beta Painter [14] .

Using a direct observation technique, the European Southern Observatory (ESO) confirmed the presence of a planet painter in the Beta system, which is consistent with earlier forecasts. The planet rotates in the plane of the disk surrounding the star. At the moment, this exoplanet is the closest to its star of those that managed to photograph. The distance between the planet and the star is approximately equal to the distance between our Sun and Saturn [15] .

Content

Location and Visibility

Beta Painter is a star in the constellation of the southern hemisphere of the sky. The painter is visible to the west of the bright star Canopus [16] . The apparent stellar magnitude of a star is 3.861 [1] , and under good weather conditions it is visible to the naked eye if light pollution does not interfere. This is the second brightest star in the constellation, which is second only to the Alpha Painter with a visible magnitude of 3.30 [17] .

The distance to the Beta Painter, as well as to many other stars, was obtained using the Hipparcos satellite , which measured their trigonometric parallaxes : slight changes in the apparent position of the star when the Earth moves around the Sun. The Beta Painter’s parallax measurement initially gave a value of 51.87 milliseconds of an arc [18] , but later, with a more careful approach to systematic errors, a specified value was found - 51.44 milliseconds of an arc [3] . The distance to the Beta Painter is estimated at 63.4 light years, with a permissible measurement error of 0.1 light years [19] [note 3] .

The Hipparcos satellite also measured the Beta Painter’s own movement : it moves eastward at a speed of 4.65 milliseconds of arc per year, and in the north - at a speed of 83.10 milliseconds of arc per year [3] . Measurements of the Doppler shift in the spectrum of the star made it possible to establish that it moves away from us at a speed of about 20 km / s [2] . Several other stars move in approximately the same direction as the Beta Painter, and probably formed almost simultaneously in the same gas cloud: this group is called the moving group of Beta Painter stars [8] .

Physical Characteristics

Spectrum, Luminosity, and Variability

In accordance with measurements made as part of the Nearby Stars project, Beta Painter belongs to the spectral class A6V [4] . The letter A means that, like Sirius or Vega , this star has a white color, which distinguishes it from our yellow Sun , which belongs to the spectral class G [20] . The number 6 indicates that the star is located approximately in the middle between the hottest stars of class A (A0) and the coldest (A9). The Roman numeral V denotes the level of luminosity and means that, like the Sun, Beta Painter is a star of the main sequence . Combustion in such stars is supported by the thermonuclear reaction of hydrogen in the nuclei.

According to the spectrum, the effective temperature of the Beta Painter is 7,779 ° C [4] , which is higher than that of the Sun (5,505 ° C [20] ). Spectral analysis also indicates a high ratio between the content of heavy elements (called "metals" in astronomy) and hydrogen - higher than on our star. This ratio, denoted by [M / H], is calculated as the decimal logarithm of the ratio of the concentration of "metals" in the star and in the Sun, in the case of Beta Painter [M / H] is 0.05 [4] , and thus the proportion of metals in the star is 12% higher than the corresponding share in the Sun [note 2] .

By analyzing the spectrum, it was possible to measure the acceleration of gravity on the surface of the star. It is usually characterized by the value of log g - the decimal logarithm of the acceleration of gravity , expressed in units of GHS , that is, in cm / s². In the case of Beta the Painter, log g = 4.15 [4] , which corresponds to 140 m / s² , which is approximately two times less than on the surface of the Sun (274 m / s²) [20] .

As a class A star of the main sequence, the Beta Painter has a greater luminosity than the Sun, since her visible magnitude of 3.861 at a distance of 19.44 parsecs from the Sun corresponds to an absolute magnitude of 2.42, while in the Sun this indicator is 4.83 [20] [21] [note 1] . This means that the luminosity of a star is 9.2 times greater than that of the Sun [note 4] . If we take into account the entire spectrum of radiation (the so-called "bolometric luminosity"), then the luminosity of Beta the Painter is 8.7 times greater than the solar [6] [22] .

Many stars of spectral class A of the main sequence are in the region of the Hertzsprung-Russell diagram , called the instability band , which is occupied by pulsating variable stars . In 2003, photometric monitoring of a star revealed fluctuations in the brightness of the star at a level of 1-2 thousandths with a frequency between 30 and 40 minutes [23] . The Beta Painter’s radial acceleration measurements also revealed variability: pulsations were detected with two different frequencies - 30.4 and 36.9 minutes [24] . Thus, the Beta Painter can be attributed to variable stars such as the Shield Delta .

Mass, Radius, and Rotation

The Beta Painter's mass was determined using a stellar evolution model applied to the observed characteristics of a star. As a result, it was found that the mass of the star is between 1.7 and 1.8 solar mass [6] . The angular size of the star was measured by interphometry using the VLT complex and turned out to be equal to 0.84 milliseconds of the arc [7] . Since the star is at a distance of 63.4 light years, with such an angular size, its radius is 1.8 of the radius of the Sun [note 5] .

The rotation speed of Beta Painter, according to measurements, is at least 130 km / s [9] . Since this value was obtained by measuring radial velocities , this is only the lower limit on the true velocity v , since the quantity v sin ( i ) is actually measured, where i is the inclination of the axis of rotation of the star relative to the line connecting it with the observer. If we assume that the Beta Painter is visible from the Earth in its equatorial plane (this is plausible, since the circumstellar disk is visible to us from the edge), then the rotation period is approximately 16 hours, that is, significantly shorter than the rotation period of the Sun (609.12 hours [ 20] ) [note 6] .

Age and Formation

The presence of a significant amount of dust near the star [25] means that the stellar system is relatively young. This caused a debate about whether the star belongs to the main sequence or has not yet reached it [26] However, when the distance to the star was calculated by the Hipparcos mission, it turned out that the Beta Painter is located farther from the Sun than previously thought, and therefore possesses greater luminosity than imagined. When the results of Hipparcos were taken into account, it turned out that the age of the Beta Painter is close to the zero age of the main sequence and, thus, it still belongs to this sequence [6] . Analysis of the Beta Painter and other members of the moving group of stars Beta Painter suggests that they are approximately 12 million years old [8] . Including errors, age can range between 8 and 20 million years [8] .

The Beta Painter and her neighbors could form near the Scorpio-Centaurus stellar association [27] . The collapse of the gas cloud that led to the formation of the Beta Painter may have been caused by a shock wave from a supernova explosion . The supernova star was probably a companion to HIP 46950 , which is now a “runaway star” like Barnard’s star . Tracking the path of HIP 46950 to the past, it can be assumed that about 13 million years ago it was near the Scorpio-Centauri association [27] .

The circumstellar environment

Shrapnel Disc

 
Hubble telescope image showing the first and second debris disks

An excess of infrared radiation from Beta the Painter was first noticed by the IRAS orbital observatory in 1983 [25] . Along with Vega , Fomalhaut and Epsilon Eridana , Beta Painter was one of the first stars to have this kind of excess: they began to be called "Vega-like" by the name of the first star of this type. Since class A stars, such as Beta the Painter, emit most of their energy in the blue spectral region [note 7] , this excess indicated the presence of cold matter in the orbit around the star, which emits in the infrared part of the spectrum and causes such an excess [25] . The hypothesis was confirmed in 1984, when the Beta Painter became the first star to have a circumstellar disk optically fixed [10] .

The fragmentary disk of Beta the Painter is visible to the observer from the Earth from the edge and is oriented in space with one edge to the south-west, and the other to the north-east. The disk is asymmetric: in the northeast direction it is observed at a distance of up to 1835 AU from the star, and in the southwest - up to 1450 a. e. [28] The disk rotates: its north-eastern part moves away from us, and the south-western part - towards us [29] .

In the outer areas of the disc, between 500 and 800 a. E., it is possible to distinguish several weakly expressed rings: according to one version, they were formed as a result of disturbances from a star flying nearby [30] . According to astrometric data obtained by the Hipparcos spacecraft, the red giant Beta Pigeon passed at a distance of two light years from Beta the Painter about 110,000 years ago, but stronger disturbances could be caused by the passage of the Zeta Golden Fish at a distance of about 3 light years about 350,000 years ago [31] . However, computer simulation indicates a longer exposure and lower speed of the perturbing object than the mentioned stars, and it can be assumed that some companion star Beta Painter, who was in an unstable orbit, generated the rings. Modeling shows that a star with a mass of 0.5 solar , probably a red dwarf of the spectral class M0V [28] [32], can be a candidate for the role of such a companion.

In 2006, observations of the system using the Hubble’s improved viewing camera revealed a second disk in the system, inclined 5 ° relative to the main one and extending 130 a. e. from the star [33] . The second disk is also asymmetric: the southwestern extremity of the disk is more curved and less inclined relative to the main disk than the northeastern one. Technical conditions of observation did not allow to resolve the primary and secondary disks closer than 80 a. e. from Beta the Painter, however, presumably, the secondary disk intersects with the main one at a distance of about 30 a. e. from the star [33] . The secondary disk could be formed due to the presence of a massive planet with an inclined orbit located in its plane, which captured part of the matter from the main disk [34] .

The observations made by NASA's FUSE spacecraft revealed the presence of an excess of carbon-rich gases in the Beta Painter's system [35] . This probably stabilizes the system from exposure to radiation pressure , which would otherwise blow matter into interstellar space. [35] At the moment, there are two hypotheses that explain the excess carbon in the system. The Beta system of the Painter may be in the process of forming exotic carbon planets , which, unlike the Earth-like planets of the Solar System, are rich in carbon and not oxygen [36] . According to another hypothesis, the system may be at a stage of formation unknown to us, through which our solar system at one time also passed: in our system there are very carbon-rich meteorites ( Enstatite chondrites ) that could form only in a carbon-rich medium. In addition, it is believed that Jupiter could form around a carbon-rich planetary core [36] .

Planesimale Belts

 
Dust in the Beta system of the Painter can be generated due to collisions of large planetesimals .

In 2003, observations of the interior of the Beta Painter's system using the Kek II telescope showed features characteristic of belts or rings of matter. The discovered belts are located at a distance of 14, 28, 52, and 82 AU from the star, and have different inclinations relative to the main disk [11] .

In 2004, observations revealed the presence of an inner silicate belt at a distance of approximately 6.4 a. e. from the star. Silicates were also found at distances of 16 and 30 a. e. Given the small amount of dust between 6.4 and 16 a. e., this may indicate the existence of a massive planet in this area [37] [38] .

Computer simulation of a dust disk at a distance of 100 AU from the star gives reason to believe that in this zone dust was formed in a series of collisions, the beginning of which is the destruction of planetesimals with radii of about 180 kilometers. After the initial collision, fragments of planetesimals continue to collide - this process is called the “collisional cascade” ( English collisional cascade ). Similar processes were recorded in dust disks around Fomalhaut and AU Microscopes [39] .

Falling and evaporating bodies

The Beta Painter’s spectrum exhibits strong short-period variability, which was initially seen in the red wings of several absorption spectral lines . This variability is supposed to be caused by the fall of matter on a star [40] . The source of this matter is considered to be small comet-like objects whose orbits come so close to the star that they begin to evaporate. Such an assumption was called the model of “falling evaporating bodies” [12] . Similar changes in the blue wings of the absorption lines were also detected, but they occur less frequently: this may mean the presence of a second group of objects in another group of orbits [41] . A detailed computer simulation showed that bodies are unlikely to consist mainly of ice, like comets, but most likely have a core of a mixture of ice and dust with a crust of refractory matter [42] . Perhaps these objects were shifted to their orbits close to the star by gravitational perturbations from a planet with a small eccentricity located at a distance of about 10 au. from the star [43] . Falling and vaporizing bodies can also be responsible for the presence of gases high above the plane of the main fragmentation disk [44] .

Planet System

 
ESO Beta Painter system photo from planet

On November 21, 2008, it was reported that during observations made in 2003 with the help of a very large telescope , the planet Beta Painter b was discovered by the star [45] . In autumn 2009, these observations were confirmed by observing the planet on the other side of the central star. Probably, after 15 years, the planet’s orbit will be fully traced [15] . The eccentricity of the orbit does not exceed 0.17. In 2014, the Gemini Planet Imager camera of the Chilean Gemini Observatory received an image of planet b [46] .

Planet
Weight
( M J )		Semimajor axis
orbits ( a.u. )
b8 +5
−2		8 +1.7
−0.4

The Doppler method , with the help of which many currently known exoplanets have been discovered, is not very suitable for studying stars of spectral class A, such as the Beta Painter, and the very young age of the star creates additional obstacles. The restrictions obtained by this method to date exclude the existence of a planet of the " hot Jupiter " class more massive than the two masses of Jupiter , closer than 0.05 a. e. from the star. A planet with a mass of less than 9 masses of Jupiter, orbiting at a distance of about 1 AU, would also not be able to detect [13] [24] . Therefore, to detect planets in the Beta system of the Painter, astronomers look for traces of the effects of the planets on the circumstellar medium.

There is a series of indications in favor of the existence of the planet at a distance of about 10 a. e. from the star: the dust-free region between the belts of planetesimals between 6.4 and 16 a. e., possibly “cleared” by the planet [38] ; a planet at such a distance could explain the origin of “falling and evaporating bodies” [43] ; in addition, the inclination and deformation of the rings in the inner disk could also be caused by a massive planet with an inclined orbit, destroying the disk [34] [47] .

 
Beta Painter b in both elongations .

The observed planet cannot explain the structure of planetesimal belts at a distance of about 30 and 52 AU from the star. These belts can be affected by planets located at a distance of 25 and 44 AU, with masses of 0.5 and 0.1 masses of Jupiter, respectively [13] . Such a system of planets, if it exists, would be close to the orbital resonance of 1: 3: 7. It is possible that the rings in the outer part of the main disk are at a distance of 500-800 AU (discussed above) are indirectly caused by the influence of these planets [13] .

As for the already known planet, it was observed at a distance of 411 milliseconds of an arc from the Beta Painter, which corresponds to a distance of 8 a. e. from the star. For comparison, the orbits of Jupiter and Saturn have a radius of 5.2 [48] and 9.5 a. e. [49], respectively. The size of the orbit in the direction of the observer is unknown, so the reduced distance is a lower estimate of the size of this orbit. Estimates of planet mass depend on the theoretical model of planetary evolution. It is believed that the object has a mass of about 8 masses of Jupiter, its temperature is about 1400-1600 K, and at the moment it is still cooling. These estimates are preliminary, since the model used to obtain them has not yet been verified on real data from the range corresponding to the probable mass and age of the planet.

Perhaps the passage of this planet through the Beta Painter’s disk was observed as far back as November 1981 [50] [51] . In this case, it is possible to clarify the dimensions of the semi-major axis - 7.6-8.7 a. e. and the orbital period - 15.9-19.5 years. The observed radius of the object during passage corresponded to 2–4 radii of Jupiter, which is more than the theoretical model suggests. This may mean that, as is possible, and in the case of Fomalhaut b , the planet is surrounded by a large system of rings or a disk in which satellites of the planet are formed [51] .

In 2014, the rotation period of β Painter b was first determined: a day on it lasts about 8 hours. [52]

Dust Flow

Observations made in 2000 by the University of Canterbury ( Christchurch , New Zealand ) revealed the existence of a stream of dust coming from the direction of the Beta Painter. This stream is probably the main source of interstellar meteoroids in our solar system [14] . Dust particles in the stream from Beta the Painter are relatively large, with radii of more than 20 micrometers , and, judging by their acceleration, they left their native system at a speed of about 25 km / s. These particles could leave the fragmentation disk during the migration of giant planets inside the disk and indirectly support the formation of an analogue of the Oort Cloud in the Beta Painter's system [53] . Numerical modeling of dust emission from the system showed that the pressure of light can be involved in this process, and found that the planets are more than 1 ao distant. e. from stars, cannot directly cause dust flow [54] .

See also

  • 51 Ophiuchus
  • List of stars of the constellation Painter
  • Moving group of stars Beta Painter

Star

  1. ↑ 1 2 The absolute magnitude M V of a star can be calculated if its apparent magnitude m V and its distance d are known using the following equation:MV=mV-fivelogten⁡(dtenparsecs) {\ displaystyle \ scriptstyle M_ {V} = m_ {V} -5 \ log _ {10} \ left ({\ frac {d} {10 \ mathrm {\ parsecs}}} \ right)}  
  2. ↑ 1 2 Calculated from [M / H]: relative prevalence = 10 [M / H]
  3. ↑ Parallax can be calculated using the following equation:Distanceinparsecs=oneparallaxinarcseconds {\ displaystyle \ scriptstyle \ mathrm {Distance \ in \ parsecs} = {\ frac {1} {\ mathrm {parallax \ in \ arcseconds}}}}  
  4. ↑ Visible luminosity can be calculated asLV∗LV⊙=ten0.4(MV⊙-MV∗) {\ displaystyle \ scriptstyle {\ frac {L_ {V _ {\ ast}}} {L_ {V _ {\ odot}}}} = 10 ^ {0.4 (M_ {V _ {\ odot}} - M_ {V _ {\ ast }})}}  
  5. ↑ The linear diameter of a star can be found by multiplying the distance to it by the angular diameter in radians .
  6. ↑ The rotation period can be calculated using the equation of circular motion :Prot=2πrvrot {\ displaystyle \ scriptstyle P _ {\ mathrm {rot}} = {\ frac {2 \ pi r} {v _ {\ mathrm {rot}}}}}  
  7. ↑ Based on the law of Wien's displacement and temperature of 8052 K , the maximum radiation of Beta Painter is 360 nanometers , that is, the ultraviolet region of the spectrum.

Notes

  1. ↑ 1 2 * bet Pic — Star (neopr.) . SIMBAD Date of treatment September 6, 2008.
  2. ↑ 1 2 Gontcharov GA HIP 27321 (neopr.) . Pulkovo radial velocities for 35493 HIP stars (2006). Date of treatment September 6, 2008. Archived March 18, 2012.
  3. ↑ 1 2 3 4 van Leeuwen, F. HIP 27321 (neopr.) . Hipparcos, the New Reduction (2007). Date of treatment September 6, 2008. Archived March 18, 2012.
  4. ↑ 1 2 3 4 5 6 7 Gray, RO et al. Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc — The Southern Sample // The Astronomical Journal : journal. - IOP Publishing , 2006. - Vol. 132 , no. 1 . - P. 161-170 . - DOI : 10.1086 / 504637 . - . - arXiv : astro-ph / 0603770 .
  5. ↑ 1 2 Hoffleit D. and Warren Jr WH HR 2020 (neopr.) . Bright Star Catalog, 5th Revised Ed. (1991). Date of treatment September 6, 2008. Archived March 18, 2012.
  6. ↑ 1 2 3 4 5 6 Crifo, F. et al. β Pictoris revisited by Hipparcos. Star properties // Astronomy and Astrophysics . - EDP ​​Sciences 1997. - Vol. 320 . - P. L29 — L32 . - .
  7. ↑ 1 2 Kervella, P. (2003). " VINCI / VLTI Observations of Main Sequence Stars " in IAUS 219: Stars as Suns: Activity, Evolution and Planets . AK Dupree and AO Benz Proceedings of the 219th symposium of the International Astronomical Union : 80, Sydney, Australia: Astronomical Society of the Pacific. Retrieved 2008-09-07 .  
  8. ↑ 1 2 3 4 5 6 Zuckerman, B. et al. The β Pictoris Moving Group (Eng.) // The Astrophysical Journal . - IOP Publishing , 2001. - Vol. 562 , no. 1 . - P. L87 — L90 . - DOI : 10.1086 / 337968 . - .
  9. ↑ 1 2 Royer F .; Zorec J. and Gomez AE HD 39060 (neopr.) . Rotational velocities of A-type stars. III. List of the 1541 B9- to F2-type stars, with their vsini value, spectral type, associated subgroup and classification (2007). Date of treatment September 7, 2008. Archived March 18, 2012.
  10. ↑ 1 2 Smith, BA and Terrile, RJ A circumstellar disk around Beta Pictoris (Eng.) // Science . - 1984. - Vol. 226 , no. 4681 . - P. 1421-1424 . - DOI : 10.1126 / science.226.4681.1421 . - . - PMID 17788996 .
  11. ↑ 1 2 Wahhaj, Z. et al. The Inner Rings of β Pictoris // The Astrophysical Journal . - IOP Publishing 2003. - Vol. 584 , no. 1 . - P. L27 — L31 . - DOI : 10.1086 / 346123 . - . - arXiv : astro-ph / 0212081 .
  12. ↑ 1 2 Beust, H .; Vidal-Madjar, A .; Ferlet, R. and Lagrange-Henri, AM The Beta Pictoris circumstellar disk. X — Numerical simulations of infalling evaporating bodies (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences 1990. - Vol. 236 , no. 1 . - P. 202-216 . - .
  13. ↑ 1 2 3 4 Freistetter, F .; Krivov, AV and Löhne, T. Planets of β Pictoris revisited ( Astronomy and Astrophysics . - EDP ​​Sciences 2007. - Vol. 466 , no. 1 . - P. 389-393 . - DOI : 10.1051 / 0004-6361: 20066746 . - . - arXiv : astro-ph / 0701526 .
  14. ↑ 1 2 Baggaley, W. Jack. Advanced Meteor Orbit Radar observations of interstellar meteoroids (English) // J. Geophys. Res. : journal. - 2000. - Vol. 105 , no. A5 . - P. 10353-10362 . - DOI : 10.1029 / 1999JA900383 . - .
  15. ↑ 1 2 Exoplanet Caught on the Move (unopened) (unavailable link) (June 10, 2010). Date of treatment June 10, 2010. Archived March 18, 2012.
  16. ↑ Kaler, Jim. Beta Pictoris (unspecified) . STARS . Date of treatment September 8, 2008. Archived March 18, 2012.
  17. ↑ Darling, David. Pictor (abbr. Pic, gen. Pictoris) (unspecified) . The Internet Encyclopedia of Science . Date of treatment September 8, 2008. Archived March 18, 2012.
  18. ↑ ESA. HIP 27321 ( unspecified ) . The Hipparcos and Tycho Catalogs (1997). Date of treatment September 7, 2008. Archived March 18, 2012.
  19. ↑ Pogge, Richard. Lecture 5: Distances of the Stars (neopr.) . Astronomy 162: Introduction to Stars, Galaxies, & the Universe . Date of treatment September 8, 2008. Archived March 18, 2012.
  20. ↑ 1 2 3 4 5 Sun Fact Sheet (neopr.) . NASA Date of treatment September 7, 2008. Archived March 18, 2012.
  21. ↑ Absolute Magnitude (neopr.) . COSMOS — The SAO Encyclopedia of Astronomy . Date of treatment September 8, 2008. Archived March 18, 2012.
  22. ↑ Strobel, Nick. Magnitude System (neopr.) . Astronomy Notes . Date of treatment September 8, 2008. Archived March 18, 2012.
  23. ↑ Koen, C. δ Scuti pulsations in β Pictoris (unknown) // MNRAS . - 2003. - T. 341 , No. 4 . - S. 1385-1387 . - DOI : 10.1046 / j.1365-8711.2003.06509.x . - .
  24. ↑ 1 2 Galland, F. et al. Extrasolar planets and brown dwarfs around A – F type stars. III. β Pictoris: looking for planets, finding pulsations (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences , 2006. - Vol. 447 , no. 1 . - P. 355-359 . - DOI : 10.1051 / 0004-6361: 20054080 . - . - arXiv : astro-ph / 0510424 .
  25. ↑ 1 2 3 Croswell, Ken. Planet Quest . - Oxford University Press , 1999. - ISBN 0-19-288083-7 .
  26. ↑ Lanz, Thierry; Heap, Sara R. and Hubeny, Ivan. HST / GHRS Observations of the beta Pictoris System: Basic Parameters of the Age of the System (Eng.) // The Astrophysical Journal : journal. - IOP Publishing 1995. - Vol. 447 , no. 1 . - P. L41 . - DOI : 10.1086 / 309561 . - .
  27. ↑ 1 2 Ortega, VG et al. New Aspects of the Formation of the β Pictoris Moving Group (Eng.) // The Astrophysical Journal : journal. - IOP Publishing 2004. - Vol. 609 , no. 1 . - P. 243-246 . - DOI : 10.1086 / 420958 . - .
  28. ↑ 1 2 Larwood, JD and Kalas, PG Close stellar encounters with planetesimal discs: the dynamics of asymmetry in the β Pictoris system (English) // MNRAS : journal. - 2001. - Vol. 323 , no. 2 . - P. 402-416 . - DOI : 10.1046 / j.1365-8711.2001.04212.x . - . - arXiv : astro-ph / 0011279 .
  29. ↑ Olofsson, G .; Liseau, R. and Brandeker, A. Widespread Atomic Gas Emission Reveals the Rotation of the β Pictoris Disk // The Astrophysical Journal : journal. - IOP Publishing , 2001. - Vol. 563 , no. 1 . - P. L77 — L80 . - DOI : 10.1086 / 338354 . - . - arXiv : astro-ph / 0111206 .
  30. ↑ Kalas, P .; Larwood, J .; Smith, BA and Schultz, A. Rings in the Planetesimal Disk of β Pictoris (Eng.) // The Astrophysical Journal . - IOP Publishing , 2000. - Vol. 530 , no. 2 . - P. L133 — L137 . - DOI : 10.1086 / 312494 . - . - arXiv : astro-ph / 0001222 .
  31. ↑ Kalas, Paul; Deltorn, Jean-Marc and Larwood, John. Stellar Encounters with the β Pictoris Planetesimal System (English) // The Astrophysical Journal : journal. - IOP Publishing , 2001. - Vol. 553 , no. 1 . - P. 410-420 . - DOI : 10.1086 / 320632 . - . - arXiv : astro-ph / 0101364 .
  32. ↑ NASA (2000-01-15). Beta Pictoris Disk Hides Giant Elliptical Ring System . Press release . Retrieved 2008-09-02 .
  33. ↑ 1 2 Golimowski, DA et al. Hubble Space Telescope ACS Multiband Coronagraphic Imaging of the Debris Disk around β Pictoris // The Astronomical Journal : journal. - IOP Publishing , 2006. - Vol. 131 , no. 6 . - P. 3109-3130 . - DOI : 10.1086 / 503801 . - . - arXiv : astro-ph / 0602292 .
  34. ↑ 1 2 NASA (2006-06-27). Hubble Reveals Two Dust Disks Around Nearby Star Beta Pictoris . Press release . Retrieved 2008-09-02 .
  35. ↑ 1 2 Roberge, Aki et al. Stabilization of the disk around β Pictoris by extremely carbon-rich gas (Eng.) // Nature : journal. - 2006. - Vol. 441 , no. 7094 . - P. 724-726 . - DOI : 10.1038 / nature04832 . - . - arXiv : astro-ph / 0604412 . - PMID 16760971 .
  36. ↑ 1 2 NASA (2006-06-07). NASA's Fuse Finds Infant Solar System Awash in Carbon . Press release . Retrieved 2006-07-03 .
  37. ↑ Okamoto, Yoshiko Kataza et al. An early extrasolar planetary system revealed by planetesimal belts in β Pictoris (English) // Nature : journal. - 2004. - Vol. 431 , no. 7009 . - P. 660-663 . - DOI : 10.1038 / nature02948 . - . - PMID 15470420 .
  38. ↑ 1 2 Burnham, Robert. Making planets at Beta Pictoris (neopr.) . Astronomy Magazine (2004). Date of treatment September 2, 2008. Archived March 18, 2012.
  39. ↑ Quillen, Alice C .; Morbidelli, Alessandro and Moore, Alex. Planetary embryos and planetesimals residing in thin debris discs (English) // MNRAS : journal. - 2007. - Vol. 380 , no. 4 . - P. 1642-1648 . - DOI : 10.1111 / j.1365-2966.2007.12217.x . - .
  40. ↑ Lagrange-Henri, AM; Vidal-Madjar, A. and Ferlet, R. The Beta Pictoris circumstellar disk. VI - Evidence for material falling on to the star // Astronomy and Astrophysics : journal. - EDP ​​Sciences 1988. - Vol. 190 . - P. 275-282 . - .
  41. ↑ Crawford, IA; Beust, H. and Lagrange, A.-M. Detection of a strong transient blue-shifted absorption component in the Beta Pictoris disc // MNRAS : journal. - 1998. - Vol. 294 , no. 2 . - P. L31 — L34 . - DOI : 10.1046 / j.1365-8711.1998.01373.x . - .
  42. ↑ Karmann, C .; Beust, H. and Klinger, J. The physico-chemical history of Falling Evaporating Bodies around beta Pictoris: investigating the presence of volatiles (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences , 2001. - Vol. 372 , no. 2 . - P. 616-626 . - DOI : 10.1051 / 0004-6361: 20010528 . - .
  43. ↑ 1 2 Thébault, P. and Beust, H. Falling evaporating bodies in the β Pictoris system. Resonance refilling and long term duration of the phenomenon (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences , 2001. - Vol. 376 , no. 2 . - P. 621-640 . - DOI : 10.1051 / 0004-6361: 20010983 . - .
  44. ↑ Beust, H. and Valiron, P. High latitude gas in the β Pictoris system. A possible origin related to falling evaporating bodies (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences 2007. - Vol. 466 , no. 1 . - P. 201-213 . - DOI : 10.1051 / 0004-6361: 20053425 . - . - arXiv : astro-ph / 0701241 .
  45. ↑ ESO (2008-11-21). Beta Pictoris planet finally imaged? . Press release . Retrieved 2008-11-22 .
  46. ↑ New Exoplanet Hunter Directly Images Alien Worlds Discovery News.htm
  47. ↑ Mouillet, D .; Larwood, JD; Papaloizou, JCB and Lagrange, AM A planet on an inclined orbit as an explanation of the warp in the Beta Pictoris disc (English) // MNRAS : journal. - 1997. - Vol. 292 . - P. 896–904 . - . - arXiv : astro-ph / 9705100 .
  48. ↑ Jupiter Fact Sheet (neopr.) . NASA Date of treatment July 10, 2009. Archived March 18, 2012.
  49. ↑ Saturn Fact Sheet (neopr.) . NASA Date of treatment July 10, 2009. Archived March 18, 2012.
  50. ↑ Lecavelier des Etangs, A. et al. Beta Pictoris light variations. I. The planetary hypothesis (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences 1997. - Vol. 328 . - P. 311-320 . - .
  51. ↑ 1 2 Lecavelier des Etangs, A. & Vidal-Madjar, A. (2009), "Is Beta Pic b the transiting planet of November 1981?" , arΧiv : 0903.1101 [astro-ph] , DOI 10.1051 / 0004-6361 / 200811528  
  52. ↑ Beta Pictoris b: Scientists Measure Spin Rate of Exoplanet for First Time , Sci-News.com (April 30, 2014).
  53. ↑ Krivova, NA and Solanki, SK A stream of particles from the β Pictoris disc: A possible ejection mechanism (Eng.) // Astronomy and Astrophysics : journal. - EDP ​​Sciences 2003. - Vol. 402 , no. 1 . - P. L5 — L8 . - DOI : 10.1051 / 0004-6361: 20030369 . - .
  54. ↑ Krivov, AV et al. Towards understanding the β Pictoris dust stream // Astronomy and Astrophysics . - EDP ​​Sciences 2004. - Vol. 417 , no. 1 . - P. 341-352 . - DOI : 10.1051 / 0004-6361: 20034379 . - .

Links

  • The Circumstellar Disk Learning Site
  • Beta Pictoris (unspecified) (link not available) . Archived on October 11, 2008.
  • Dr. David Jewitt's page on Beta Pic , 1997
  • Beta Pictoris on SolStation
  • ARICNS (unopened) (inaccessible link) . Archived on June 9, 2007.
  • SEDS entry ( unopened ) (inaccessible link) . Archived December 9, 2005.
  • Notes for star Beta Pictoris
Source - https://ru.wikipedia.org/w/index.php?title= Beta of the Painter &oldid = 100073973


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