12 Boötis

12 Boötis
12 Boötis
Classificazionebianco-gialla nella sequenza principale
Classe spettraleF8IV / F9IVw
Distanza dal Sole120 anni luce
CostellazioneBoote
Redshift10,80 ± 0,90
Coordinate
(all'epoca J2000.0)
Ascensione retta14h 10m 23,9336s
Declinazione+25° 05′ 30,037″
Lat. galattica+72,1762°
Long. galattica030,8219°
Dati fisici
Raggio medio2,47 / 1,86[1] R⊙
Massa
1,42 / 1,37[1] M⊙
Acceleraz. di gravità in superficie3,73 logg
Temperatura
superficiale
  • 6130 / 6230 K[1] (media)
Luminosità
0,89 / 0,67[1] L⊙
Metallicità93% del Sole
Dati osservativi
Magnitudine app.4,82
Magnitudine ass.2
Parallasse27,27 ± 0,78 mas
Moto proprioAR: -23,02 ± 0,73 mas/anno
Dec: -60,07 ± 0,47 mas/anno
Velocità radiale10,8 ± 0,9 km/s
Nomenclature alternative
d Boötis, HD 123999, GSC 02010-01245, PMC 90-93 372, TYC 2010-1245-1, HIC 69226, PPM 103125, UBV M 20016, HIP 69226, ROT 2031, UBV 12491, AG +25 1460, HR 5304, SAO 83203, uvby98 100123999, BD +25 2737, IRAS 14081+2519, SBC7 510, WDS J14104+2506, FK5 522, JP11 2476, SBC9 804, YZ 25 6736, GC 19127, 2MASS J14102394+2505301, [HFE83] 1010, GCRV 8301, N30 3215, SRS 30522, PLX 3221, TD1 17295
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12 Boötis è una stella bianco-gialla nella sequenza principale di magnitudine 4,82 situata nella costellazione di Boote. Dista 120 anni luce dal sistema solare.

Osservazione

Si tratta di una stella situata nell'emisfero celeste boreale; grazie alla sua posizione non fortemente boreale, può essere osservata dalla gran parte delle regioni della Terra, sebbene gli osservatori dell'emisfero nord siano più avvantaggiati. Nei pressi del circolo polare artico appare circumpolare, mentre resta sempre invisibile solo in prossimità dell'Antartide. La sua magnitudine pari a 4,8 fa sì che possa essere scorta solo con un cielo sufficientemente libero dagli effetti dell'inquinamento luminoso.

Il periodo migliore per la sua osservazione nel cielo serale ricade nei mesi compresi fra fine marzo e agosto; da entrambi gli emisferi il periodo di visibilità rimane indicativamente lo stesso, grazie alla posizione della stella non lontana dall'equatore celeste.

Caratteristiche fisiche

La stella è una binaria spettroscopica formata da due stelle simili fra loro, di classe F8IV e F9IV, dunque entrambe subgiganti. Il periodo orbitale del sistema è di 9,6 giorni e la distanza media tra le due componenti di 0,1245 UA[1].

Possiede una magnitudine assoluta di 2 e la sua velocità radiale positiva indica che la stella si sta allontanando dal sistema solare.

Note

  1. ^ a b c d e Accurate masses and radii of normal stars (Torres+, 2010)

Voci correlate

Collegamenti esterni

  Portale Stelle: accedi alle voci di Wikipedia che trattano di stelle e costellazioni

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