白矮星 的英文怎麼說
中文拼音 [báiǎixīng]
白矮星
英文
[天文學] white dwarf-
As a slowly contracting dwarf the star may remain luminous for billions of years.
收縮較慢的白矮星仍會發光幾十億年。The nova phenomenon generally occurs in a binary system that has as one member a very hot white dwarf.
新星這種現象一般發生在雙星系統中，其中一顆子星是非常熱的白矮星。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。Measuring 2, 500 miles across and weighing five million trillion trillion pounds, the rock was found on valentine ' s day buried in the core of a white dwarf star in the constellation centaurus
這塊石頭直徑達2500英里，重5 10的42次方磅，藏在人馬座中一顆白矮星的中心，是在情人節那天被發現的。This and the x - ray spectrum, which exhibits a high concentration of iron atoms relative to oxygen and silicon, convincingly show that the ejecta are the remains of an exploded white dwarf star
這幅圖連帶x射線光譜（顯示出了鐵相對氧與硅的高度集中）令人信服地說明，拋出的物質是爆發白矮星的殘余。Ben oppenheimer led the research team that discovered the white dwarfs
本?奧本海姆領導發現這些白矮星的研究小組。Mister oppenheimer says most of the white dwarfs may be about ten - thousand - million years old
奧本海姆先生說，大多數白矮星大約有100億歲。In general, ba stars belong to binary system, and their heavy - element overabundances are due to the accreting material from the companions ( the former tp - agb stars and the present white dwarfs ). carrying out a series of monte - carlo simulations, the changes of orbital elements of binaries are recalculated for wind accretion scenario of the total angular momentum conservation
研究表明，鋇星應該屬于雙星系統，其重元素超豐來自雙星吸積，它的伴星已經經歷了s -過程核合成，而且由在以前發生的同其伴星（以前是agb星，現已演化為白矮星）的質量傳輸過程中，從伴星那裡獲得了富含重元素的物質，這樣造成了鋇星的重元素超豐。White dwarfs provide an important beginning for understanding the material in this chapter.
白矮星是掌握本章材料的重要出發點。White dwarfs compact much of the mass of the stars into a volume the size of the earth.
白矮星將其大部分質量緊密地聚集在相當地球大小的范圍內。Such diverse objects as red giants and white dwarfs would seem to be genetically related to each other.
象紅巨星和白矮星這樣迥然不同的天體，竟然彼此之間有起源上的聯系。It will quietly and steadily burn the hydrogen to helium and become a white dwarf
它會穩定地把氫轉化為氦，然後安靜的死去，成為白矮星。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？Since a 7 - solar - mass is too large to be a white dwarf or neutron star, it must be a black hole
因為有著7個太陽質量的星體不可能是白矮星或中於星，所以它一定是黑洞。Topics include : planets, planet formation ; stars, the sun, " normal " stars, star formation ; stellar evolution, supernovae, compact objects ( white dwarfs, neutron stars, and black holes ), plusars, binary x - ray sources ; star clusters, globular and open clusters ; interstellar medium, gas, dust, magnetic fields, cosmic rays ; distance ladder ; galaxies, normal and active galaxies, jets ; gravitational lensing ; large scaling structure ; newtonian cosmology, dynamical expansion and thermal history of the universe ; cosmic microwave background radiation ; big - bang nucleosynthesis
課程的主題包含了：行星、行星形成；恆星、太陽、正常的恆星、恆星形成；恆星演化、超新星、緻密天體（白矮星、中子星及黑洞） 、波霎、雙x -射線源；星團、球狀及疏散星團；星際介質、氣體、塵埃、磁場、宇宙射線；距離階梯；星系、正常及活躍星系、噴流；重力透鏡；大尺度結構；牛頓宇宙學、宇宙的動力膨脹及溫度發展歷史；宇宙背景微波輻射；大霹靂核合成。If the mass of the white dwarf becomes greater than about 1. 4 times the mass of the sun, it becomes unstable and is blown apart in a thermonuclear explosion
如果白矮星的質量超過了太陽的1 . 4倍，它會變得不穩定，並在熱核爆炸中碎裂。A few stars on the road to dwarfhood flare up briefly from time to time.
有些星星在演變為白矮星的過程中，不時地隱隱閃爍。As the main-sequence mass of the star increases, the mass of the final remnant left as a white-dwarf star also increases.
在恆星在主序的質量增加時，作為白矮星留下來的最終殘骸的質量也增加。After it has radiated away all its residue energy, it becomes a
當白矮星把所有能量輻射完畢，它便會成為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。分享友人