27 Рака

27 Рака
Звезда
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Наблюдательные данные
(Эпоха J2000.0)
Прямое восхождение 8ч 26м 43,94с[1]
Склонение +12° 39′ 16,59″[1]
Расстояние 281,096 ± 10,3194 пк[1]
Видимая звёздная величина (V) 5,5[2]
Созвездие Рак
Астрометрия
Лучевая скорость (Rv) −8,39 ± 0,53 км/с[3]
Собственное движение
 • прямое восхождение −18,617 ± 0,153 mas/год[1]
 • склонение −103,771 ± 0,134 mas/год[1]
Параллакс (π) 3,5575 ± 0,1306 mas[1]
Абсолютная звёздная величина (V) −1,95
Спектральные характеристики
Спектральный класс M3IIIa[4]
Показатель цвета
 • B−V 1,6
 • U−B 1,92
Переменность SRB полуправильная[5][6]
Физические характеристики
Радиус 119 R☉
Светимость около 515 L☉
Коды в каталогах

GSC 00804-01492, 2MASS J08264391+1239169, HD 71250, HIP 41400, HR 3319, IRAS 08239+1249, SAO 97819, BD+13 1912, CSV 1302, FK5 2658, GC 11525, GCRV 5573, HIC 41400, IRC +10189, JP11 1676, PLX 2007, PLX 2007.00, PPM 125269, RAFGL 1255, TYC 804-1492-1, BP Cnc, YZ 12 3403, DO 2504, WEB 8007, Gaia DR2 650828355848334080, 27 Cnc, Gaia DR3 650828355848334080, TIC 7024474, AAVSO 0821+13, AG+12 1032 и UBV M 14318

Информация в базах данных
SIMBAD * 27 Cnc
Логотип Викиданных Информация в Викиданных ?

27 Рака (27 Cancri) − красный гигант класса М. Находится в 1050 световых годах от нашей Солнечной системы. Это пульсирующая переменная звезда, яркость которой колеблется от +5,41 до +5,75 звёздной величины.

Наблюдение

Звезда расположена в северном небесном полушарии, недалеко от небесного экватора, что делает её доступной для наблюдения почти со всей Земли, кроме Антарктиды. Малый блеск звезды на небе (+5,56) делает её трудной для наблюдения невооружённым глазом, и вблизи источников искусственного освещения.

Наилучший период для наблюдений складывается с декабря по май.

Физические характеристики

27 Рака является красным гигантом с переменной яркостью. Среднее значение абсолютной звёздной величины составляет −1,95 и означает что, звезда светит в 515 раз ярче нашего Солнца. Её отрицательная радиальная скорость указывает на приближение звезды к Земле.

Согласно исследованиям, звезда является частью потока Арктура — группы звёзд с высокой скоростью собственного движения и низкого уровня металличности, которая, возможно, является остатками галактики, поглощённой Млечным Путём[7].

Примечания

  1. ↑ 1 2 3 4 5 6 Gaia Early Data Release 3 (англ.) / Data Processing and Analysis Consortium, European Space Agency — 2020.
  2. ↑ Ducati J. R. Catalogue of Stellar Photometry in Johnson's 11-color system (англ.) — 2002. — Vol. 2237.
  3. ↑ Gaia Data Release 3 (англ.) / Data Processing and Analysis Consortium, European Space Agency — 2022.
  4. ↑ Keenan P. C., McNeil R. C. The Perkins catalog of revised MK types for the cooler stars (англ.) // The Astrophysical Journal: Supplement Series — AAS, 1989. — Vol. 71. — P. 245–266. — ISSN 0067-0049; 1538-4365 — doi:10.1086/191373
  5. ↑ Samus N. N., Durlevich O. V., et a. General Catalogue of Variable Stars (Samus+ 2007-2011) — 2009. — Т. 1. — С. 2025.
  6. ↑ SIMBAD Astronomical Database
  7. ↑ Eggen, Olin. The Arcturus Group (англ.) // Publications of the Astronomical Society of the Pacific. — 1971. — Vol. 83, no. 493. — P. 271—285. — doi:10.1086/129120. — Bibcode: 1971PASP...83..271E. Архивировано 2 июля 2019 года.

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