Delta Crucis

Delta Crucis
Delta Crucis
ClassificazioneStella bianco-azzurra di
sequenza principale
Classe spettraleB2IV
Tipo di variabileBeta Cephei
Distanza dal Sole345 anni luce
CostellazioneCroce del Sud
Coordinate
(all'epoca J2000)
Ascensione retta12h 15m 8,7s
Declinazione-58° 44′ 56″
Dati fisici
Raggio medio4,9 R⊙
Massa
8,5 M⊙
Temperatura
superficiale
Luminosità
5600 L⊙
Età stimata18 milioni di anni[2]
Dati osservativi
Magnitudine app.
  • +2,78 (media)
Magnitudine app.2,752
Magnitudine ass.-2,33[3]
Parallasse8,96 ± 0,60 mas
Moto proprioAR: -36,68 mas/anno
Dec: -10,72 mas/anno
Velocità radiale+22,2 km/s
Nomenclature alternative
9 Corvi, HR 4656, HD 106490, HIP 59747, SAO 239791
Modifica dati su Wikidata · Manuale

Delta Crucis o Decrux è la quarta stella più luminosa della costellazione della Croce del Sud. La sua magnitudine apparente è +2,78 e dista all'incirca 345 anni luce dal sistema solare[3].

Osservazione

Essendo una stella del cielo australe è visibile dall'emisfero sud e dalle regioni tropicali boreali della Terra, mentre più a nord della latitudine 32°N non è mai visibile. Dall'emisfero australe diventa circumpolare più a sud del parallelo 32°S, cioè dal Cile, dall'Argentina, dall'Uruguay e dalle zone meridionali di Sudafrica e Australia. Delle quattro stelle che compongono l'asterismo della Croce del Sud è la più occidentale e la più debole, dopo Mimosa, Acrux e Gacrux. Avendo un magnitudine apparente di +2,78 la stella è facilmente individuabile anche dai piccoli centri urbani parzialmente affetti da inquinamento luminoso.

Dati fisici

Decrux è una stella azzurra di tipo spettrale B2IV, con una temperatura superficiale di 22.500 K. Si tratta di una stella giovane, con non più di 30 milioni di anni, ed anche se dal suo spettro parrebbe una subgigante, che avrebbe cioè terminato l'idrogeno da fondere nel suo nucleo, analisi della sua temperatura e della sua luminosità suggeriscono invece che si tratti di una stella che è solo a metà della sua vita nella sequenza principale. Delta Crucis è 8,9 più massiccia del Sole[2] e la sua luminosità, comprendendo la radiazione ultravioletta, è 5600 volte superiore[4].

Il suo tipo spettrale è simile a quello delle vicine Acrux e Mimosa (Becrux) e si pensa che nonostante non siano legate gravitazionalmente le tre stelle abbiano origini comuni. Come Becrux è anch'essa una variabile Beta Cephei, con un piccolo cambio di luminosità in un periodo di 3,7 ore.

Note

  1. ^ N.A. Sokolov, The determination of T_eff_ of B, A and F main sequence stars from the continuum between 3200 A and 3600 A (PDF), in Astronomy and Astrophysics Supplement, Maggio 1995.
  2. ^ a b Tetzlaff, N et al., A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun, in Monthly Notices of the Royal Astronomical Society, vol. 410, n. 1, gennaio 2011, pp. 190–200, DOI:10.1111/j.1365-2966.2010.17434.x.
  3. ^ a b Erik Anderson, Charles Francis, XHIP: An Extended Hipparcos Compilation, in Astronomy Letters, 23 marzo 2012.arΧiv:1108.4971
  4. ^ (EN) Jim Kaler, DELTA CRU, su stars.astro.illinois.edu. URL consultato il 22 gennaio 2012 (archiviato dall'url originale il 6 febbraio 2012).

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