4 Cassiopeiae

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32k JPEG M103 (NGC581) is a pretty large (6'), round, rich open cluster 1° NW of Delta Cassiopeiae. Total brightness is mag. Stars range from mags. Image taken with a HISYS 22 (two minute exposure) on a 4' Meade at f6.3. Let’s begin with an easy one, the fine double star η (eta) Cassiopeiae. Also called Achird, it’s one of the most colorful and appealing doubles anywhere in the sky. The primary star shines at magnitude 3.5 with a yellow-gold color. Even very bright Gamma Cassiopeiae has none, at least in western lore. Pity then the seemingly lesser stars, which have no chance at all. At least in one spectacular case, however, the 'lesser' tag is totally wrong. Look to fifth magnitude (4.54, just over the line from fourth) Rho Cas, way down on the Bayer Greek Letter list. Beta Cassiopeiae is known as Caph from the Arabic meaning ‘stained hand’, because the stars of Cassiopeia were thought by the Arabs to represent a hand tattooed with henna. Delta Cassiopeiae is named Ruchbah, from the Arabic for ‘knee’, rukbat. The central star of the W, Gamma Cassiopeiae, is an erratic variable star, given to.

4 Cassiopeiae is a wide binary star^[8] system in the northern constellation of Cassiopeia,^[7] located approximately 790 light-years away from the Sun.^[1] It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96.^[2] At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust.^[9] This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.^[5]

The primary member of this system, component A, is an evolvedred giant star, currently on the asymptotic giant branch,^[4] with a stellar classification of M2− IIIab.^[2] It is a suspected variable star of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00.^[3] As of 2011, the magnitude 9.88 secondary, component B, lay at an angular separation of 96.10″ along a position angle of 226° relative to the primary.^[10] In the sky, the open cluster Messier 52 is 40' to the south of it, near the constellation border with Cepheus.

References[edit]

1. ^ ^abcdefvan Leeuwen, F. (2007). 'Validation of the new Hipparcos reduction'. Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID18759600.
2. ^ ^abcdefAnderson, E.; Francis, Ch. (2012), 'XHIP: An extended hipparcos compilation', Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID119257644.
3. ^ ^abcSamus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), 'General catalogue of variable stars', Astronomy Reports, 5.1, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID125853869.
4. ^ ^abEggen, O. J. (1992), 'Asymptotic giant branch stars near the sun', The Astronomical Journal, 104: 275, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
5. ^ ^abFamaey, B.; et al. (2009), 'Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations', Astronomy and Astrophysics, 498 (2): 627–640, arXiv:0901.0934, Bibcode:2009A&A...498..627F, doi:10.1051/0004-6361/200810698, S2CID18739721.
6. ^Pasinetti Fracassini, L. E.; et al. (February 2001), 'Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)', Astronomy and Astrophysics (Third ed.), 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID425754.
7. ^ ^ab'4 Cas'. SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-13.
8. ^Eggleton, P. P.; Tokovinin, A. A. (September 2008), 'A catalogue of multiplicity among bright stellar systems', Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID14878976.
9. ^Famaey, B.; et al. (January 2005), 'Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters', Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID17804304.
10. ^Mason, B. D.; et al. (2014), 'The Washington Visual Double Star Catalog', The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.

NASA
Eta Cassiopeiae A is a yellow-orange
star like our Sun, Sol. (See a 2MASS
Surveyimage of Eta Cassiopeiae from
the NASA Star and Exoplanet Database.)

System Summary

Also called Achird, Eta Cassiopeiae (Eta Cas) is located about 19.4 light-years (ly) from our Sun, Sol. It can be found in the central part (00:49:06.29+57:48:54.67, ICRS 2000.0) of Constellation Cassiopeia, the Lady of the Chair -- northeast of Schedar (Alpha Cassiopeiae) and southwest of Mu Cassiopeiae. This well known binary star system was discovered in 1779 by Sir William Friedrich Wilhelm Herschel (1738-1822, portrait), who subsequently discovered the planet Uranus in 1781 -- which led to his appointment in 1782 as private astronomer to the King of England.

© 2001-2005 Kevin Muenzler,
Eagle Creek Observatory
(used with permission).
Larger image.
The orange tint of Eta Cas B can
be detected in this photo (more).

Due to Eta Cassiopeiae's relative proximity and similarity of spectral type to Sol, the star has been an object of intense interest among astronomers. Eta Cassiopeiae became one of the top 100 target stars for NASA's proposed Terrestrial Planet Finder (TPF), but the project has been postponed indefinitely. It was also selected as a 'Tier 1' target star for NASA's optical Space Interferometry Mission (SIM) to detect a planet as small as three Earth-masses within two AUs of its host star (and so some summary system information and images of Eta Cassiopeiae A and B may still be available from the SIM Teams), but the SIM project manager announced on November 8, 2010 that the mission was indefinitely postponed due to withdrawal of NASA funding.

JPL, CalTech, NASA
Larger illustration
Astronomers have identified Eta Cas A
as a prime target for the Terrestrial Planet
Finder (TPF), and the Space Interferometry
Mission (SIM), now both indefinitely postponed.

AB Binary Star System

According to a 1969 article by Kaj Aage Gunnar Strand (1907-2000; obit), Star A and B are separated by an 'average' distance of 71 times the Earth-Sun distance (AU) (of a semi-major axis). They move in an eccentric orbit (e= 0.497) of about 480 years, so that the two stars get as close as 36 AUs and as far away as 107 AUs. Their orbit is inclined by almost 35 degrees from Earth's line of sight. Based on chromospheric activity and rotational period alone, both stars may be around 2.9 and 5.8 billion years old (Mamajek et al, 2008, Table 13). Star A, however, is no longer thought to have a spectroscopic binary companion with a nine-day orbital period (Morbey and Griffin, 1987; and Helmut Abt, 1987).

---------------------------------------------- [Guide] -- [Larger] ----------------------------------------------

The main sequence yellow-orange primary (G3 V) may have about 90 to 111 percent of Sol's mass (RECONS; Allende Prieto and Lambert, 1999; and Daniel M. Popper, 1980), almost the same diameter -- 98 to 101 percent (Johnson and Wright, 1983, page 647; and Daniel M. Popper, 1980; or Petr Harmanec, 1988), and 1.2 times its luminosity. It is about 63 to 68 percent as enriched as Sol in elements heavier than hydrogen (metallicity), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 5). Some useful catalogue numbers for this star are: Eta Cas, 24 Cas, HR 219, Gl 34 A, Hip 3821, HD 4614, BD+57 150, SAO 21732, LHS 123, LTT 10287, LFT 74, Wolf 24, Struve 60, and ADS 671 A.

Estimates provided by the NASA Star and Exoplanet Database indicate that the inner edge of Eta Cassiopeiae's habitable zone could be located around 0.90 AU from the star, while the outer edge edge lies around 1.80 AUs. The distance from Star A where an Earth-type planet could have liquid water on its surface is centered around 1.35 AU -- between Earth's and somewhat short of Mars' orbital distance of 1.5 AUs in the Solar System. At that distance from Star A and assuming that it has 1.1 Solar-mass, such a planet would have an orbital period of just under 1.5 years.

This cooler and dimmer, main sequence orange-red dwarf star (K7 V) may have 56 to 60 percent) of Sol's mass (RECONS; and Daniel M. Popper, 1980), 66 percent of its diameter (Johnson and Wright, 1983, page 647), and only around three percent of its luminosity. Radial velocity variations have been detected (Andrei A. Tokovinin, 1992). Useful catalogue numbers for this star include: Gl 34 B, LHS 122, and ADS 671 B.

© Torben Krogh & Mogens Winther,
(Amtsgymnasiet and EUC Syd Gallery,
student photo used with permission)
Eta Cassiopeiae B ia a orange-red
dwarf star, like Epsilon Eridani at
left center of meteor

With a spectral type of K7, 41 Arae B can be used as a rough proxy for Eta Cass B (K1). According to calculations performed for the NASA Star and Exoplanet Database, the distance from 41 Arae B where an Earth-type rocky planet may have liquid water on its surface has been estimated to be between 0.593 and 1.176 AU -- between the orbital distances of Mercury and Earth in the Solar System. In that distance range from the star, such a planet would have an orbital period shorter an Earth year. For an Earth-type planet, the orbital distance where it would have liquid water zone on its surface would be around 0.884 AU, where the orbital period would be 392 days (1.073 years) if the star actually does have around 60 percent of a Solar-mass.

An attempt to find large planets from December 1986 to February 1987 failed to detect large periodic variations in radial velocities (McMillan and Smith, 1987; more discussion at Hatzes et al, 2004). A subsequent search ruled out close-orbiting giant planets and similar objects at least as large as 0.878 Jupiter-mass in circular orbits within three AUs of Star A (Wittenmyer et al, 2006, Table 5).

Closest Neighbors

4 Cassiopeiae Exhaust

The following star systems are located within 10 ly of Eta Cassiopeiae 2.

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4 Cassiopeiae Lane

4 Cassiopeiae Words

4 Cassiopeiae 3

Other Information

4 Cassiopeiae Equals

• Try Professor Jim Kaler's Stars site for other information about Achird at the University of Illinois' Department of Astronomy.

• Up-to-date technical summaries on this star can be found at: the Astronomiches Rechen-Institut at Heidelberg's ARICNS for Star A and Star B, the NASA Star and Exoplanet Database, and the Research Consortium on Nearby Stars (RECONS) list of the 100 Nearest Star Systems. Additional information may be available at Roger Wilcox's Internet Stellar Database.

• With its stars shaped in a 'W,' this northern constellation was named by the Ancient Greeks for the mother of Andromeda who claimed to be more beautiful than the daughters of Nereus, a god of the sea. Cassiopeia's vanity so angered the sea god Poseidon that he had Andromeda chained to a rock of the coast as a sacrifice for Cetus (the monstrous whale) until Perseus rescued her. For more information on stars and other objects in this Constellation and a photograph, go to Christine Kronberg's Cassiopeia. For an illustration, see David Haworth's Cassiopeia.

• For more information about stars including spectral and luminosity class codes, go to ChView's webpage on The Stars of the Milky Way.