矮星

爆炸后所留下的是一个密度巨大的矮星。

What is left after an explosion is a dwarf star of extraordinary density .

新发现的X射线选活动星系核、白矮星和激变变星

Discovery of X-ray Selected AGNs , a White Dwarf and a Cataclysmic Variable

他们认为这个庞大的物体是由两颗“白矮星”合并而成的，通常白矮星会以强大的超新星的形式爆炸。这颗新星被天文学家称为“白矮星”。

The new star is what astronomers1 call a ' white dwarf2 ' .

一些白矮星的大气中几乎只有纯氢或氦，但这颗星的大气中重元素碳的含量异常高。

Some white dwarves4 have almost pure hydrogen or helium atmospheres , but this star has an atmosphere unusually high in the heavier element , carbon .

太阳附近G矮星金属含量分布和化学演化

G Dwarfs Metallicity Distribution in the Solar Neighbourhood and the Chemical Evolution

解决G矮星问题的银河系化学演化三成分模型

Solving the G-dwarf Problem with a Three-Component Model of the Chemical Evolution of the Galaxy

DA型和非DA型白矮星的目视表面亮度和半径的关系

Visual surface brightness and radius of Da and non-DA white dwarfs

这一褐矮星已经被正式编号为WISEJ104915.57-531906。

And it 's been dubbed WISE J085510.83-071442.5 .

WISE和Spizer的红外线镜也只能依稀辨别褐矮星微弱的光芒。

Its dim thermal glow was just barely discernible to the infrared eyes of WISE and Spitzer .

相反，来自双白矮星并合的超新星产生的X射线辐射要比吸积少很多。

A supernova from a merger of two white dwarfs , on the other hand , would create significantly less X-ray emission than the accretion scenario .

剩下的开放问题是，在旋涡星系中，这些并合的白矮星是否就是Ia型超新星的主要催化剂。

An open question remains whether these white dwarf mergers are the primary catalyst for Type1a supernovae in spiral galaxies .

去年在弗吉尼亚州夏洛茨维尔，国家射电天文台（NationalRadioAstronomyObservatory）的天文学家发现了一颗脉冲星，绕着它运动的另外两颗缩小的恒星被称为白矮星，而这一现象是前所未见的。

Last year , astronomers at the National Radio Astronomy Observatory in Charlottesville , Virginia , discovered the first pulsar orbited by two other shrunken stars , called white dwarfs .

一个碳氧白矮星可以通过洛希瓣物质交流或者通过星风从其伴星吸积物质，从而增加自身质量，最终由于不稳定的热核燃烧而发生Ia型超新星爆炸。

A carbon-oxygen white dwarf may explode as Type Ia supernova by accreting matter from its company via either Roche lobe overflow or wind .

观测结果还首次显示，白矮星在爆炸成为Ia型超新星之前，会在其周围创造一个空洞。

The observations also show for the first time that a white dwarf can create a cavity around it before blowing up in a Type Ia event .

美国航空航天局的科学家借助WISA和Spitzer太空望远镜观测到了褐矮星。

It was spotted recently by NASA 's WISE and Spitzer space telescopes .

大多数科学家认为，当白矮星（年老恒星坍缩而成的残骸）超过质量极限，变得不稳定并爆发的时候，会产生Ia型超新星。

Most scientists agree a Type1a supernova occurs when a white dwarf star a collapsed remnant of an elderly star exceeds its weight limit , becomes unstable and explodes .

与星族Ⅰ恒星相反，贫金属的星族Ⅱ的F和早型G型矮星大气锂丰度弥散很小，且其丰度比年轻的星族Ⅰ恒星和星际介质锂的丰度约低一个量级。

In . contrast with Pup I stars the Li abundances of Pup ⅱ F - and early G-type dwarfs show a very small dispersion and they are about an order of magnitude smaller than the value of the young Pup I stars .

我们在双星演化程序中加入了吸积盘不稳定性的因素，并采用最新的白矮星表面的H和He稳定燃烧的条件，以此未跟踪不同初始质量和轨道周期的白矮星双星的演化。

We include the effect of unstable accretion disk to binary evolution code , and the latest description of H and He burning condition at the surface of white dwarfs to follow the evolution of white dwarf binaries with different initial masses and orbital periods .

科学家发现了数颗围绕着长蛇座M矮星GJ357运行的系外行星，系外行星指的是围绕太阳系外恒星运行的行星。

Multiple exoplanets -- planets orbiting stars outside our solar system -- were discovered orbiting an M-dwarf star , called GJ 357 in the Hydra constellation .

这种方法最初是利用元素对Th/Nd来确定G矮星的年龄，近年来开始利用元素对Th/Eu和U/Th来确定晕族场星和球状星团内恒星的年龄。

At first , this age-dating approach was used to estimate the age of G-dwarf stars with Th / Nd chronometry . Recently , it has been used to evaluate the age of halo field stars and globular cluster stars with the Th / Eu and U / Th chronometers .

而红矮星Gliese581位于天秤星座，距离地球20光年，大约比太阳昏暗50倍。

The star is located 20 light-years from Earth in the constellation Libra . Red dwarf stars are about 50 times dimmer than our sun .

那两个最像地球的行星分别是Kepler-438b和Kepler-442b。它们都绕红矮星轨道运行。这些恒星（红矮星）不仅比太阳小，还比太阳冷。

The two most Earth-like planets , known as Kepler-438b and Kepler-442b , both orbit red dwarf stars that are smaller and cooler than the sun .

Gliese581g是环绕红矮星Gliese581两颗行星中的其中一颗，它的发现使该行星系内行星数量增加至6颗。

Gliese 581g is one of two new worlds the team discovered orbiting the red dwarf star Gliese 581 , bumping that nearby star 's family of planets to six .

这一新发现的行星被称为LHS1140b，与其母星的距离是地球与太阳距离的十分之一，但由于红矮星比身为黄矮星的地球要冷得多，所以该行星还是位于宜居带。

The new world - dubbed LHS 1140b - is ten times closer to its parent star than Earth but because a red dwarf is far cooler than our own yellow dwarf , the planet still sits in the habitable zone .

但是PNES理论的基本原理和思路与原有的理论完全不同，按照原有理论，白矮星系统只是一种电子系统，氦离子系统只被视为约束电子系统的外部约束条件。

According as the original theory has regarded the white dwarf star system is a electron system alone , the helium-ion system is only looked as a external condition that the electron system is restricted .

将一个新理论&正、负能谱（PNES）热力学理论应用于白矮星系统的力学平衡问题，对白矮星初期演化阶段的力学平衡进行了详细的分析。

Applying the new theory-the positive and negative energy spectrum ( PNES ) thermodynamical theory to the mechanical equilibrium of white dwarf stars , the mechanical equilibrium of white dwarf star at early stage has been analysed carefully .

正是距离产生诱惑，天文学家对白矮星关爱有加。

And that distance is what makes white dwarves so attractive .

白矮星的平衡质量上限

The Upper-limit of the Equilibrium Mass of the White Dwarf Star

这意味着，白矮星并合是这些星系中的主导过程。

This implies that white dwarf mergers dominate in these galaxies .

Ⅰ型超新星模型&部分燃尽白矮星

Models for Type I Supernovae : Partially Incinerated White Dwarfs