例句與造句

1. In stars of, a pulsational pair-instability supernova can occur.
2. Pulsational pair-instability supernovae are likely the most common pair-instability events and are probably common causes of supernova impostor events.
3. Stars above will generally produce much greater levels of electron-positron pairs and will usually produce more than just that required of a pulsational pair-instability supernova.
4. Stars of 130 to will often undergo pulsational pair-instability supernovae and potentially undergo more than one pulsation to bring its mass under although they can potentially go full supernova.
5. Like full scale pair-instability supernovae, pulsational pair-instability supernova are very bright and last for many months longer than a typical type II or type I supernova.
6. It's difficult to find pulsational in a sentence. 用pulsational造句挺難的
7. By analysing its radial velocity from its spectrum, Pugh and colleagues calculated a period of 5.93 ?0.01 years and considered whether this change was orbital or pulsational.
8. For Betelgeuse, the total mass lost is predicted to be no more than about, giving a current mass of, considerably higher than estimated by other means such as pulsational properties or limb-darkening models.
9. Possible examples of pulsational pair-instability supernovae include the 1843 eruption of Eta Carinae A, and possibly SN 1000 + 0216 which could have been either a pulsational pair-instability supernova or a supernova of pair-instability.
10. Possible examples of pulsational pair-instability supernovae include the 1843 eruption of Eta Carinae A, and possibly SN 1000 + 0216 which could have been either a pulsational pair-instability supernova or a supernova of pair-instability.
11. As a result, the likely outcome will be a pulsational pair-instability supernova, in which the star will eject a large amount of its mass, which will generally bring it under where it will typically undergo a normal core-collapse supernova . [ 2 ] [ 1]
12. This was confirmed in 1953 by American astronomer D . Harold McNamara, who identified it as a Beta Cephei variable . ( At the time he actually identified it as a Beta Canis Majoris star, which was subsequently designated a Beta Cephei variable . ) It has a radial pulsation period of 0.15175 days ( 3.642 hours ), but also shows the behavior of a slowly pulsating B star ( SPB ) with three additional pulsational frequencies.