Phecda

Phecda
Le stelle del Grande Carro
ClassificazioneStella bianca di sequenza principale
Classe spettraleA0Ve SB
Distanza dal Sole84 ± 1 anni luce
CostellazioneOrsa Maggiore
Coordinate
(all'epoca J2000.0)
Ascensione retta11h 53m 49,8s
Declinazione+53° 41′ 41″
Dati fisici
Raggio medio3,04[1] R⊙
Massa
Velocità di rotazione178 km/s
Temperatura
superficiale
  • 9320 K (media)
Luminosità
Indice di colore (B-V)0,00
Età stimata415 milioni di anni[2]
Dati osservativi
Magnitudine app.+2,41
Magnitudine ass.+0,38
Parallasse38,99 ± 0,68 mas
Moto proprioAR: 107,8 mas/anno
Dec: 11,16 mas/anno
Velocità radiale−13 km/s
Nomenclature alternative
Phecda, Phekda, Phad, Phegda, Phekha, Phacd, Fekda γgamma; UMa, 64 UMa, HR 4554, HD 103287, BD+54 1475, FK5 447, HIP 58001, SAO 28179, GC 16268
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Phecda (γ UMa / γ Ursae Majoris / Gamma Ursae Majoris) è una stella situata nella costellazione dell'Orsa Maggiore. Il nome tradizionale, noto anche nelle varianti Phekda e Phad, deriva dalla parola araba فخذ fakhdh [faxð], "coscia" (del Grande Orso).

L'astro è familiare alla gran parte degli osservatori dell'emisfero boreale, in quanto fa parte dell'asterismo del Grande Carro, di cui costituisce il vertice sudorientale. Assieme a quattro altre stelle di questo famoso asterismo Phecda costituisce un'associazione stellare nota come associazione dell'Orsa Maggiore.

Osservazione

Si tratta di una stella situata nell'emisfero boreale. La sua posizione è fortemente boreale e ciò comporta che la stella sia osservabile prevalentemente dall'emisfero nord, dove si presenta circumpolare anche da gran parte delle regioni temperate; dall'emisfero sud la sua visibilità è invece limitata alle regioni temperate inferiori e alla fascia tropicale. La sua magnitudine pari a +2,41 fa sì che possa essere scorta anche con un cielo affetto da inquinamento luminoso.

Caratteristiche fisiche

Phecda è propriamente una stella bianca di classe spettrale A0 Ve; si tratta quindi di una stella che, come buona parte delle stelle della nostra Galassia, si trova nella sequenza principale, una lunga fase di stabilità durante la quale fonde l'idrogeno del nucleo in elio. Phecda è 2,4 volte più massiccia del Sole, 75 volte più luminosa e con un raggio 3 volte superiore. Lo spettro della stella è caratterizzato dalla presenza di linee di emissione (indicate dalla "e" nella classe spettrale), che la rendono affine alle più calde stelle Be[4].

Note

  1. ^ E. L. Fitzpatrick, D. Massa, Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry, in The Astronomical Journal, vol. 129, n. 3, marzo 2005, pp. 1642–1662, Bibcode:2005AJ....129.1642F, DOI:10.1086/427855.
  2. ^ a b Jeremy Jones et al., The ages of a-stars. i. interferometric observations and age estimates for stars in the Ursa Major moving group, in The Astrophysical Journal, vol. 813, n. 1, 2015.
  3. ^ Rotational velocities of A-type stars. IV. (Zorec+, 2012)
  4. ^ (EN) Jim Kaler, Pechda, su stars.astro.illinois.edu, Università dell'Illinois.

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