Stage 3 - In the next million years a series of nuclear reactions occur forming different elements in shells around the iron core. Stage 4 - The core collapses in less than a second, causing an explosion called a Supernova, in which a shock wave blows of the outer layers of the star. ...
In the previous chapter we saw how astrophysics grew from the need to understand how stars are constructed and how we can use astrophysics to deduce the internal conditions of stars from their visible properties鈥攊ncluding their mass, their size, and their luminosity (their surface temperature, ...
In subject area:Physics and Astronomy Young Stellar Objects are very young stars that display typical features such as a flared circumstellar accretion disk and highly collimated jets, as seen in the case of the 'young stellar object' HH30 in Taurus. ...
Astronomy and AstrophysicsL. B. van den Hoek, W. J. G. de Blok, J. M. van der Hulst, and T. de Jong, "The evolution of the stellar populations in low surface brightness galaxies," Astronomy & Astrophysics, vol. 357, no. 2, pp. 397-413, 2000....
In examining astronomers' reconstructions of stellar evolution, I have been struck by a number of similarities between ways stars and societies have evolved. The parallels actually begin with the method used by both disciplines, namely, the comparative method. In astronomy, the method involves ...
Stellar evolution - the birth, development and death of stars - is central to our current understanding of astronomy. This area of astrophysics is often portrayed as being difficult and mathematical, but Mike Inglis brings it to life in a unique way, combining a step-by-step introduction with...
Herwig,Falk - 《Annual Review of Astronomy & Astrophysics》 被引量: 521发表: 2005年 Principle of Stellar Evolution and Nucleosynthesis Donald D. Clayton's Principles of Stellar Evolution and Nucleosynthesis remains the standard work on the subject, a popular textbook for students in astron... DD...
必应词典为您提供stellar-evolution的释义,un. 星体演化; 网络释义: 恒星演化;恒星的演化;演化生命的尽头;
The evolution of helium white dwarfs: I. The companion of the\n millisecond pulsar PSR J1012+5307 We present a grid of evolutionary tracks for low-mass white dwarfs with helium cores in the mass range from 0.179 to 0.414 Msol. The lower mass limit is we... D Schrock - 《Astronomy &...
After a star has formed and is on the "main sequence" in its evolution, it will be fusing hydrogen in its core. Hydrogen is the simplest form of atom, with one positively charged particle called a proton orbited by a negatively charged electron, although the electron is lost due to the...