supernova explosion 中文意思是什麼
supernova explosion
解釋
超新星爆發-
There is a good chance that this outward diffusion of neutrinos and antineutrinos plays a crucial role in the supernova explosion.
中微子和反中微子的這種向外的散射很可能在超新星爆發中起著關鍵的作用。 -
The supernova explosion disrupts the binary.
超新星爆發會瓦解雙星系統。 -
Data from the chandra observation show that the central ten - million - degree celsius cloud is the remains of a supernova explosion that destroyed a white dwarf star
來自錢德拉的觀測數據表明，中心溫度達上千萬攝氏度的雲湍團是超新星爆發的殘余，爆發摧毀了一顆白矮星。 -
Speculation into the cause of the rings includes beamed jets emanating from a dense star left over from the supernova, and a superposition of two stellar winds ionized by the supernova explosion
這些奇特環狀結構起源的諸多臆測，包括由緻密遺骸的高能噴流束及兩個重疊的恆星風受到超新星爆炸的游離。 -
Fig 3 : the supernova remnant n63a is believed to be left behind after the explosion of a star with 50 solar mass
圖三：超新星殘骸n63a ，相信為一顆五十倍太陽質量的恆星爆炸所遺留。 -
Recall that type i supernova is the strong explosion of a nova that even the white dwarf is destroyed
還記得i型超新星是足以令中心白矮星炸毀的新星爆發嗎？ -
Supernova explosion at song dynasty and the principle of constancy of light velocity
宋代超新星爆發事件與光速不變原理 -
The crab nebula is the remnant of the supernova explosion in 1054
蟹狀星雲是1054年超新星爆發后的遺骸 -
The crab nebula is the remnant of a star s supernova explosion which was recorded in 1054 by chinese astronomers
中國古代的天文學家在1054年記錄了一次超新星爆發，爆炸的殘骸便是現在的蟹狀星雲。 -
Perhaps the most famous pulsar lies within the crab nebula, the remnant of a supernova explosion that was observed in 1054
最有名的波霎，或許要算是蟹狀星雲里頭的那顆了，這片星雲是1054年觀測到的超新星爆炸的殘骸。 -
What will happen to the remains of the supernova explosion
恆星在超新星爆發后又如何呢？ -
Cas a is the 300 - year - old remnant created by the supernova explosion of a massive star
仙后座a是有著300年歷史的遺跡，成因是大質量恆星的超新星爆發。 -
In contrast, a type i supernova is an ordinary nova explosion that are strong enough to destroy the white dwarf at the center
Ii型超新星i型超新星其實只是強度足以把中心白矮星炸毀的普通新星爆發。 -
In fact, the cosmic crab is now known to be a supernova remnant, an expanding cloud of debris from the death explosion of a massive star
實際上，現在我們知道蟹狀星雲是超新星爆發的遺跡，即一個巨大恆星死亡后爆炸的殘屑雲。 -
After a supernova explosion, a small but compact star, called neutron star
超新星爆炸后可能會剩下一個細小但密度很高的星球，稱為中子星 -
Nature of the universe - chapter seventeen if the remnant of a supernova explosion is heavier than two or three solar masses, the neutron degenerate pressure is not strong enough to support the star. there does not exist stronger force up to our knowledge and we believe the remnant will collapse to a black hole
在超新星爆發后，如果恆星剩餘質量超過二或三個太陽質量，中子簡並壓力亦不足以抵抗向內的引力，這時在已知的物理理論裏面，再沒有更強的力能足以與引力一決雌雄，恆星只可以不斷塌縮，成為黑洞。 -
If the mass of the core after a supernova explosion is more than 1. 4 but less than about 3 solar masses, then electron degenerate pressure is not strong enough to support the star. the star will contract to a size even smaller than the white dwarf. the electrons are squeezed into the nuclei and are combined with the protons to form neutrons
假若在超新星爆發后，剩餘核心質量介乎太陽質量的1 . 4至3倍，那麼核心中的電子簡並壓力便再不足以抵抗強大的引力，恆星會進一步收縮，直至電子亦被擠壓至原子核內，和質子結合成為中子。 -
Our model introduces the general equations of chemical evolution used in galaxies to studies of gcs. in this model the important gas outflow caused by the supernova explosion and other processes during the formation of globular clusters is included. based on such a self - enrichment model, monte carlo method is used to simulate the formation and chemical evolution of globular cluster systems, from which a new explanation of the bimodal metallicity distribution can be given
本文把星系演化中通用的化學演化方程引入到球狀星團這一系統中來，特別考慮到球狀星團中恆星形成過程中超新星爆發等因素引發的氣體外流，把這一重要的物理過程包含到化學演化方程中，並用蒙特卡羅方法來模擬球狀星團系統的自增豐演化。 -
The one - million - second image shows a bright outer ring ( green ) ten light years in diameter that marks the location of a shock wave generated by the supernova explosion
曝光100萬秒的圖象揭示出了直徑10光年的明亮外環（綠色） ，這里標志著超新星爆發產生的激波起源。 -
About two years after the discovery of the supernova explosion sn1987a, kristian et al. 1989 claimed to have discovered within this sn1987a a 0. 5 ms optical pulsar which was disproved about one year later
在發現sn1987a超新星爆發兩年後，基斯坦和他的同僚宣稱他們在sn1987a內發現了一顆自轉周期為0 . 5毫秒的的脈沖星。
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