50 Perseus, 50 Persei , abbrev. 50 Per ) is a star in the northern constellation Perseus . A star has a visible magnitude of +5.52 m [2] , and, according to the Bortl scale , is visible to the naked eye even in a bright suburban sky ( English Bright suburban sky ). From parallax measurements obtained during the Hipparcos mission [1] , it is known that the star is removed at about 68.5 St. years ( 21.0 pc ) from Earth . The star is observed north of 52 ° S , i.e. It is visible practically on the entire territory of the inhabited Earth , with the exception of the polar regions of Antarctica , as well as the southernmost regions of Chile , Argentina, and Australia [13] . The best time to watch is November [13] .
| 50 Perseus | |||
|---|---|---|---|
| Star | |||
   | |||
| Observational data ( Age J2000.0 ) | |||
| Type of | Single star | ||
| Right ascension | |||
| Declination | |||
| Distance | 68.5 ± 0.4 St. years (21.0 ± 0.1 pc ) [a] | ||
| Visible magnitude ( V ) | 5.52 [2] | ||
| Constellation | Perseus | ||
| Astrometry | |||
| Radial velocity ( R v ) | +26.2 [3] km / s | ||
| Own movement (μ) | RA: +164.10 [1] Dec: −202.60 [1] | ||
| Parallax (π) | 47.63 ± 0.26 [1] mas | ||
| Absolute magnitude (V) | 3.87 [5] | ||
| Specifications | |||
| Spectral class | F7V [6] | ||
| Color Index ( B - V ) | +0.54 [2] | ||
| Color Index ( U - B ) | +0.00 [2] | ||
| Variability | RS CVn / BY Dra | ||
| physical characteristics | |||
| Weight | 1.16 [7] M ☉ | ||
| Radius | 1.34 [8] R ☉ | ||
| Age | ~ 0.6 billion [9] years | ||
| Temperature | 6147 [7] K | ||
| Luminosity | 2.47 [11] L ☉ | ||
| Metallicity | −0.11 [7] | ||
| Rotation | 20.81 [10] | ||
| |||
| Database Information | |||
| SIMBAD | |||
The star itself moves faster relative to the Sun than the other stars, its radial heliocentric speed: +25 km / s [13] , which is 2.5 times faster than the speed of the local stars of the Galactic disk , and this also means that the star is moving away from the Sun.
Star Name
50 Perseus - ( Latinized version of the lat. 50 Persei ) is the designation of Flemstead . The star also has an alternative name: V582 Perseus, V582 Per [8] .
Star Properties
50 Perseus is a dwarf of spectral class F7V [6] , which indicates that the hydrogen in the star’s core serves as nuclear “fuel”, that is, the star is in the main sequence . A star radiates energy from its external atmosphere at an effective temperature of about 6147 K [7] , which gives it the characteristic yellow-white color of a star of spectral class F.
The mass of the star is usual for a dwarf and is: 1.16 
The star has a surface gravity of 4.35 GHS [7] or 223 9 m / s 2 , i.e. slightly less than on the Sun ( 274.0 m / s 2 ). Stars with planets tend to be more metallic than the Sun, but 50 Perseus has a quarter less metallicity : the iron content in it relative to hydrogen is 78% [7] of the solar.
The rotation speed is estimated at 20.81 km / s [10] , which gives a rotation period of less than four days. 50 Perseus has an excess of infrared radiation at a wavelength of 70 μm , which indicates the presence of a circumstellar residual disk , which has a temperature of 96 ± 5 K [9] . The age of the Perseus 50 system is about 0.6 billion years [9] .
In 1998, the star was classified as a potential variable of the Golden Fish type γ with a period of 3.05 days [5] , which would mean that it shows changes in luminosity due to nonradial pulsations in the photosphere. Subsequently, the star was reclassified by the automatic program as a variable of type RS Hounds Dogs and BY Dragon , i.e. variations in its brightness arise due to rotation, since spots on its surface are similar to solar spots but occupy a much larger area, as well as due to chromospheric activity [14] .
The history of studying the multiplicity of a star
The discoverer of the multiplicity of the Perseus 50 system is considered Struve , who authorized the stars in 1851 and cataloged the AB and AC stars. The triple star itself entered catalogs under the name STT 531. Then, in 1878, S. Burnham discovered the CD star, and the fourth star itself entered catalogs under the name BU 545. And finally, in 1991, the fifth component of the system was discovered . According to the Washington catalog of visual binary stars , the parameters of these components are given in the table [15] :
| Component | Year | Position angle | Angular distance | Visible magnitude of 1 component | Visible magnitude 2 component |
| Ab | 1851 | 146 ° | 3.4 | 7.32 m | 9.69 m |
| 2015 | 353 ° | 2.9 | |||
| AC | 1851 | 205 ° | 239.8 | 7.32 m | 8.81 m |
| 2015 | 217 ° | 225.1 | |||
| Ae | 1991 | 100 ° | 746.1 | 7.32 m | 5.57 m |
| 2017 | 100 ° | 746.0 | |||
| CD | 1878 | 310 ° | 1.0 | 8.81 m | 10.71 m |
| 2015 | 315 ° | 1.2 |
However, the star does not seem to have satellites. Although four satellites are listed in the table (9th magnitude 50 Perseus B at a distance of 2.9 ", 8th magnitude 50 Perseus C at a distance of 225.1", 5th magnitude 50 Perseus E at a distance of 746 "and 10th magnitude 50 Perseus CD) their movements show that these stars move very fast, and most likely they have no gravitational connection with 50 Perseus, i.e. they are all on the line of sight.
Most likely, 50 Perseus belongs to the Hyada star cluster , whose age is estimated at 0.625 million years and which, most likely, was formed from the same gas cloud as the Crèche cluster [16] . Now the Hyada cluster is breaking up and the stars are losing gravitational connectivity. However, 50 Perseus can still have a gravitational connection in the form of tidal interaction even with the Chapel , despite the fact that now they are separated by almost 15 °, which is equivalent to a distance of more than 19 St. years ( 5.9 pc ). Also, 50 Perseus can be a dual system paired with an as yet undiscovered close companion. A star can also be physically associated with the probable binary system Perseus V491 ( HIP 19255 ). Perseus V491 components have an angular distance of 3.87 ″, and these two components rotate around each other with a period of approximately 590 years [17] . Themselves 50 Perseus and V491 Perseus are separated from each other at an angular distance of 745.98 ″ (12.4 '), as well as a distance of approximately 15,200 AU , or 0.24 St. years [17] . 50 Perseus and V491 Perseus revolve around each other with a period of approximately 1.0 million years [17] . The further fate of the Perseus 50 – V491 Perseus system is decay, especially if there will be a lot of subhalo of dark matter locally: companions will be torn off more quickly and evidence of the existence of a binary star system will be lost [17] .
Nearest star environment
The following stellar systems are within 20 light-years [18] of the 50 Perseus star (included only: the closest star, the brightest (<6.5 m ) and noteworthy stars). Their spectral classes are shown against the background of the colors of these classes (these colors are taken from the names of the spectral types and do not correspond to the observed colors of stars):
| Star | Spectral class | Distance, st. years old |
| V491 Perseus | G5 v | 0.24 [17] . |
| Chapel | K0IIIe + G1III | 19 [17] |
Near the star, at a distance of 20 light-years , there are about 10 red , orange dwarfs and yellow dwarfs of spectral class G, K and M, as well as 2 stars of spectral class F which are not on the list.
Notes
Comments
- ↑ Distance calculated by the given parallax value
- ↑ The angular diameter (δ) is calculated by the formula:
- where D S is the diameter of the star, expressed in a.u. ; d CZ - distance to habitat zone
Sources
- ↑ 1 2 3 4 5 6 ( van .) Van Leeuwen, F. ( 2007 ), " Validation of the new Hipparcos reduction ", Astronomy and Astrophysics T. 474 (2): 653-664 , DOI 10.1051 / 0004-6361: 20078357
- ↑ 1 2 3 4 (English) Mermilliod, J.-C. ( 1986 ), Compilation of Eggen's UBV data, transformed to UBV (unpublished)
- ↑ Nordström, B .; Andersen, J .; Holmberg, J. & Jørgensen, BR ( 2004 ), " The Geneva-Copenhagen survey of the Solar Neighborhood. Ages, metallicities, and kinematic properties of ~ 14000 F and G dwarfs ", Publications of the Astronomical Society of Australia T. 21 ( 2): 129–133 , DOI 10.1071 / AS04013
- ↑ 1 2 3 4 Gaia Data Release 2 - 2018.
- ↑ 1 2 (Eng.) Aerts, C. & Eyer, L., Kestens, E. ( September 1998 ), "The discovery of new gamma Doradus stars from the HIPPARCOS mission", Astronomy and Astrophysics T. 337: 790–796
- ↑ 1 2 (English) Maldonado, J .; Martínez-Arnáiz, RM; Eiroa, C. & Montes, D. ( October 2010 ), " A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups ", Astronomy and Astrophysics T. 521: A12 , DOI 10.1051 / 0004-6361 / 201014948
- ↑ 1 2 3 4 5 6 7 (English) Chen, YQ; Nissen, PE; Zhao, G. & Zhang, HW ( February 2000 ), “ Chemical composition of 90 F and G disk dwarfs ”, Astronomy and Astrophysics Supplement T. 141: 491-506 , DOI 10.1051 / aas: 2000124
- ↑ 1 2 3 50 Persei (inaccessible link - history ) . Universe Guide .
- ↑ 1 2 3 (Eng.) Beichman, CA; Bryden, G .; Stapelfeldt, KR & Gautier, TN ( December 2006 ), " New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets ", The Astrophysical Journal T. 652 (2): 1674–1693 , DOI 10.1086 / 508449
- ↑ 1 2 (Eng.) Martínez-Arnáiz, R .; Maldonado, J .; Montes, D. & Eiroa, C. ( September 2010 ), " Chromospheric activity and rotation of FGK stars in the solar proximity. An estimation of the radial velocity jitter ", Astronomy and Astrophysics T. 520: A79, doi : 10.1051 / 0004 -6361/200913725 , < http://eprints.ucm.es/37826/1/davidmontes17libre.pdf >
- ↑ 1 2 50 Persei Internet Stellar Database .
- ↑ (English) * 50 Per - Variable of RS CVn type , Center de Données astronomiques de Strasbourg , < http://simbad.u-strasbg.fr/simbad/sim-id?Ident=50+Per > . Retrieved January 27, 2019.
- ↑ 1 2 3 HR 1278 . A catalog of bright stars .
- ↑ Dubath, P .; Rimoldini, L .; Süveges, M. & Blomme, J. ( 2011 ), " Random forest automated supervised classification of Hipparcos periodic variable stars ", Monthly Notices of the Royal Astronomical Society T. 414 (3): 2602-17 , DOI 10.1111 / j.1365 -2966.2011.18575.x
- ↑ Vizier catalog entry
- ↑ The Hyades, Melotte 25 (Information from the SEDS website) . Archived on May 16, 2008.
- ↑ 1 2 3 4 5 6 (English) Shaya, Ed J. & Olling, Rob P. ( January 2011 ), " Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalog ", The Astrophysical Journal Supplement T. 192 (1): 17, 2 , DOI 10.1088 / 0067-0049 / 192/1/2
- ↑ Stars within 20 light-years of 50 Persei: (English) . Internet Stellar Database .