HR 5256

HR 5256
HR 5256
ClassificazioneNana arancione
Classe spettraleK3 V
Distanza dal Sole32.869 ± 0.008 ly
CostellazioneOrsa Maggiore
Coordinate
(all'epoca J2000.0)
Ascensione retta13h 57m 32,0592s
Declinazione+61° 29′ 34.2994″
Dati fisici
Raggio medio0,78 R⊙
Massa
0,82 M⊙
Acceleraz. di gravità in superficie4,57 cgs
Velocità di rotazione4,6 km/s
Temperatura
superficiale
  • 4811 K (media)
Luminosità
0,28 L⊙
Indice di colore (B-V)1,01
Metallicità0,17 [Fe/H]
Età stimata5,36 miliardi di anni
Dati osservativi
Magnitudine app.6,52
Magnitudine ass.6,51
Parallasse99.2285 ± 0.0232 arcsec
Moto proprio−32.074±0.063 arcsec/anno
Velocità radiale−26.376±0.0011 km/s
Modifica dati su Wikidata · Manuale

HR 5256 è una stella nana arancione situata nella costellazione circumpolare settentrionale dell'Orsa Maggiore, ad una distanza di circa 33 anni luce dal Sole.[1]

Caratteristiche

Ha una tonalità arancione e, avendo una magnitudine apparente di 6,52, è difficile da avvistare ad occhio nudo.[2] La distanza da questa stella è molto vicina a 10 parsec, quindi la magnitudine assoluta di 6,51[3] è quasi la stessa della magnitudine apparente della stella. HR 5256 si sta avvicinando al Sole con una velocità radiale di 26,4 km/s,[1] e raggiungerà la massima vicinanza al Sole tra circa 333.000 ± 16.000 anni, quando sarà ad una distanza di 12,72 ± 0,65 anni luce.[4]

Questo corpo celeste è una stella K V con una classificazione stellare di K3 V,[5] la quale indica che è in fase di fusione di idrogeno. Ha più di cinque miliardi di anni e gira lentamente con una velocità di rotazione prevista di 4,6 km/s.[3] Si stima che la stella abbia l'82%[3] della massa del Sole e il 78% del suo raggio.[6] Irradia solo il 28% della luminosità solare dalla sua fotosfera ad una temperatura efficace di 4.811 K.[3]

Note

  1. ^ a b (EN) Anthony Brown, Gaia Data Release 2: Summary of the contents and survey properties, in Astronomy and Astrophysics, vol. 616, agosto 2018, Bibcode:2018A&A...616A...1G, DOI:10.1051/0004-6361/201833051.
  2. ^ (EN) Tõnis Oja, UBV photometry of stars whose positions are accurately known. VI, in Astronomy and Astrophysics Supplement Series, vol. 89, pp. 415-419, Bibcode:1991A&AS...89..415O.
  3. ^ a b c d (EN) R. Earle Luck, Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants, in The Astronomical Journal, vol. 153, n. 1, 21 dicembre 2016, pp. 21, Bibcode:2003A&A...406..995M, DOI:10.3847/1538-3881/153/1/21.
  4. ^ (EN) C. A. L. Bailer-Jones, J. Rybizki, R. Andrae e M. Fouesneau, New stellar encounters discovered in the second Gaia data release, in Astronomy and Astrophysics, vol. 616, Bibcode:2018A&A...616A..37B, DOI:10.1051/0004-6361/201833456.
  5. ^ (EN) P. M. Marrese, F. Boschi e U. Munari, High resolution spectroscopy over 8500-8750 Å for GAIA - IV. Extending the cool MK stars sample, in Astronomy and Astrophysics, vol. 406, n. 3, 1º agosto 2003, pp. 995-999, Bibcode:2003A&A...406..995M, DOI:10.1051/0004-6361:20030647.
  6. ^ (EN) Genya Takeda, Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog, in The Astrophysical Journal Supplement Series, vol. 168, febbraio 2007, Bibcode:2007ApJS..168..297T, DOI:10.1086/509763.
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