恆星演化學 的英文怎麼說

中文拼音 [héngxīngyǎnhuàxué]
恆星演化學 英文
astrogony
  • 恆 : Ⅰ形容詞1 （永久; 持久） permanent; lasting 2 （平常; 經常） usual; common; constant Ⅱ名詞1 （恆心...
  • 星 : 名詞1 （夜晚天空中閃爍發光的天體） star 2 [天文學] （宇宙間能發射光或反射光的天體） heavenly body...
  • 演 : 動詞1 （演變; 演化） develop; evolve 2 （發揮） deduce; elaborate 3 （依照程式練習或計算） drill;...
  • 學 : Ⅰ動詞1 （學習） study; learn 2 （模仿） imitate; mimic Ⅱ名詞1 （學問） learning; knowledge 2 （學...
  • 恆星 : [天文學] fixed star; star恆星大氣 stellar atmosphere; 恆星導航 star navigation; stellar guidance;...
  1. Evolution of stars of all masses takes place on a hydrodynamic time scale.

    各種質量的恆星的演化，均以流體力學的時間尺度進行。
  2. On the bases of the galaxy evolution theory, we use the therotical chemical evolution model of three zone ( such as halo, thick disk and thin isk ) and multi - phase ( diffuse gas, molecular clouds, stars of both low and high mass, the remnants ). by comparing with the observational constraints, such assurface densities, age - metallicity relation, g - dwarf metallicity distribution in the solar neighbourhood and the correlation between [ a / fe ] and [ fe / h ], supernovae rates, infall rates. the rationality of the model is verified. based on the theory model, we calculate the abundance of neutron capture element

    本文正是在銀河系化學演化的基礎上，利用銀河系的三成分（ threezone ） （即暈、厚盤和薄盤）多相（ multi - phase ） （氣體，分子云，大、小質量恆星以及剩餘物質）的化學演化的理論模型，通過與觀測約束（質量面密度、場星的年齡-金屬豐度關系、太陽附近g矮星金屬含量分佈函數、三成份的特徵量、元素的星系化學演化、超新星的爆炸率、內落速率等）的比較，來檢驗模型的合理性。
  3. Many planets ( for example, ganymede, mercury, the earth, jupiter and saturn ) and stars ( for example, the sun ) possess intrinsic magnetic fields. the explanation for their existence and variation remains a great challenge to planetary scientists and astrophysicists. this article attempts to review some recent developments and difficulties in the study of magnetohydrodynamics for the electrically conducting fluid interiors of planets and stars. it is the fluid motions, usually driven by thermal convection, that generate and sustain magnetic fields through magnetohydrodynamic processes in planets and stars. in planets, the magnetohydrodynamic processes are strongly affected by the combined and inseparable effects of rotation, magnetic fields and spherical geometry. the key dynamics involves the interaction between the coriolis and lorentz forces. in the sun, it is the solar tachocline, a thin shear flow layer located at the base of the convection envelope, that plays an essential role in the solar magnetohydrodynamic processes which produce the 11 - year sunspot cycle. some results of a new nonlinear three - dimensional solar dynamo model are also presented

    許多行星（如木衛三，水星，地球，木星和土星）和恆星（如太陽）具有內部磁場.對這些磁場的存在和變化的解釋對行星科學家和天體物理學家是一個巨大的挑戰.本文試圖總結行星和恆星的導電流體內部磁流體力學研究的新近發展和困難.一般由熱對流驅動的流動通過磁流體力學過程產生並維持在行星和恆星中的磁場.在行星中磁流體力學過程強烈地受到轉動，磁場和球幾何位型的綜合影響.其動力學的關鍵方面涉及科里奧利力和洛倫茲力間的相互作用.在太陽中其流線，即處于對流層的薄的剪切流層在太陽的磁流體力學過程中扮演了一個基本的角色，並由之產生了11年的太陽黑子周期.本文也給出了一個新的非線性三維太陽發電機模型
  4. 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。
  5. The aim of the galaxy chemical evolution research is to reproduce the element abundance patter of stars and gas in the galaxy

    銀河系化學演化研究的任務，從根本來說，是重現銀河系中恆星與氣體的元素豐度分布圖象。
  6. The evolution time in our calculation is chosen to be 12 gyr, which is the mean value of globular cluster ages in the galaxy

    恆星蒸發對小質量球狀星團的演化起著主導作用，大質量恆星的演化、銀河系核球和盤的沖擊加熱以及動力學磨擦則主要影響大質量球狀星團的演化。
  7. Because the photospheric temperature of carbon stars are less than 3000k and the temperature of rich - dust envelope formed by the mass loss is lower, and therefore most of the energy from carbon stars are radiated between 1 to 60um range, in which the vibrational and ro - vibrational bands of many molecules also lies, the study of infrared spectra in this wavelength range is very important to reveal chemical compositions, dust formation process, the atmospheric structure and evolutionary status of stars

    碳星光球的有效溫度不超過3000k ，同時較大的質量損失率形成了富碳的塵埃殼層，以致於它的輻射能量主要集中在1 ? 60 m的紅外波段上，並且許多分子的轉動振動能譜也集中在紅外，因此在紅外波段的研究對揭示碳星化學成份及其分佈、塵埃形成過程、恆星大氣結構和演化狀態都有十分重要的意義。
  8. Simple laws of physics suggest, that gas-dust complexes in the interstellar medium may evolve, first into protostars and subsequently into stars.

    簡單的物理學定律揭示出，星際介質中的氣塵復合體可以進化，先是演化為原恆星，接下去再演化為恆星。
  9. Among the evolution is the chemical evolution of the galaxy showing its exceeding importance. the recognize to the galaxy chemical evolution build up the basement of understanding the whole galaxy evolution. and it can restrict and constrain the evolution and ncleosyhthesis of the stellar

    其中銀河系的化學演化在其中更是具有極其重要的地位，對銀河系化學演化的認識是理解整個銀河系演化的基礎，並對恆星演化與核合成理論提供約束。
  10. They are the stellar evaporation in the tidal field, the stellar evolution during the early evolutionary stage, the tidal shocks due to clusters passing through the bulge and disk, and the dynamical friction

    本文考慮的動力學過程有四種，即：恆星蒸發、早期大質量恆星的演化、銀河系核球和盤的沖擊加熱以及動力學磨擦。
  11. 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。
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