另眼看宇宙之星系和超新星合辑

Tycho's Supernova Remnant:
Chandra's View of Tycho's Supernova Remnant

第谷超新星遗迹：钱德拉眼中的第谷超新星遗迹
来源:http://chandra.harvard.edu/photo/2002/0005/index.html

This Chandra image reveals fascinating details of the turbulent debris created by a supernova explosion that was observed by the Danish astronomer Tycho Brahe in the year 1572. The colors show different X-ray energies, with red, green, and blue representing low, medium and high energies, respectively. The image is cut off at the bottom because the southernmost region of the remnant fell outside the field of view of the detector.

钱德拉拍摄的这张照片所揭示的是超新星爆发产生的混乱残片的迷人细节。1572年，丹麦天文学家第谷·布拉赫观测到了这颗超新星。颜色表示不同的X射线能段，红、绿、蓝色分别表示低能、中能和高能部分。照片的下方被截去的原因是，遗迹的最南端不在探测器的视场之内。

A shock wave produced by the expanding debris is outlined by the strikingly sharp blue circular arcs of twenty million degree Celsius gas seen on the outer rim. The stellar debris, which has a temperature of about ten million degrees and is visible only in X-rays, shows up as mottled yellow, green and red fingers of gas.

外缘醒目锐利的蓝色圆弧勾勒出了膨胀的碎片做产生的激波，圆弧是温度达到2000万摄氏度的气体。星辰的碎片有着1000万度的温度，只能通过X射线看到，就是图中斑驳的黄色、绿色和红色气体指状物。

Tycho's supernova remnant presents several interesting contrasts with the Cassiopeia A (Cas A) supernova remnant. The debris for Tycho is distributed in clumps rather than knots as in Cas A, and its outer shock wave can be seen in smooth and continuous arcs rather than being fragmented, as in Cas A.

与仙后座A（Cas A）相比，第谷超新星遗迹有着几个有趣的不同之处。第谷遗迹中的残片呈团块状分布，而非Cas A中的扭结，而其外侧的激波也不象Cas A那样破碎，而是呈现出光滑连续的圆弧。

Also, no central point source is detected in Tycho, in contrast to Cas A. The absence of a central point source is consistent with other evidence that Tycho is a Type Ia supernova, which is thought to signal the detonation and destruction of a white dwarf star. Theory predicts that a white dwarf star will explode when infalling matter from a companion star increases the mass of the white dwarf beyond a critical mass limit, known as the Chandrasekhar limit.

此外，与Cas A不同的是，第谷遗迹也没有中央点源。中央点源的缺席与其他证据一致，表明第谷遗迹源于Ia型超新星爆发。人们认为此类超新星是白矮星爆炸毁灭的标志。理论预言，当来自伴星的物质让白矮星的质量增加到了临界质量极限即钱德拉塞卡极限时，白矮星就会爆发。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 11:49 编辑 ]

DEM L71: Supernova Origin Revealed

DEM L71：揭示超新星的起源

来源:http://chandra.harvard.edu/photo/2003/deml71/index.html

NASA's Chandra X-ray Observatory image (left panel) of the supernova remnant DEM L71 reveals a hot inner cloud (aqua) of glowing iron and silicon surrounded by an outer blast wave. This outer blast wave is also visible at optical wavelengths (right panel). 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.

NASA的钱德拉X射线天文台拍摄的超新星遗迹DEM L71 的照片（左图）展现了内区热云（浅绿色），是炽热的铁与硅，包在外围激波中。外圈激波在可见光波段（右图）仍旧可见。来自钱德拉的观测数据表明，中心温度达上千万摄氏度的云湍团是超新星爆发的残余，爆发摧毁了一颗白矮星。

DEM L71 presents a textbook example of the double-shock structure expected to develop when a star explodes and ejects matter at high speeds into the surrounding interstellar gas. The expanding ejecta drive an outward-moving shock wave that races ahead of the ejecta into the interstellar gas (bright outer rim). The pressure behind this shock wave drives an inward-moving shock wave that heats the ejecta, seen as the aqua cloud.

DEM L71是双激波结构的标准范例，人们认为其产生于恒星爆发并以高速向周围星际气体抛射物质的时候。膨胀的抛出物驱动着外行激波，领先于抛出物冲入星际气体（明亮的外缘）。激波后的压力驱使内行激波加热物质，也就是图中浅绿色的云团。

The clear separation of the shocked matter and the heated ejecta in the Chandra image allowed astronomers to determine the mass and composition of the ejecta. The computed ejected mass was found to be comparable to the mass of the Sun. 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. The size and temperature of the remnant indicate that it is several thousand years old.

在钱德拉的照片上，激波扰过的物质与被加热的抛出物之间明显的分隔让天文学家可以定出抛出物的质量与组分。算出的抛出物质量与太阳相当。这幅图连带X射线光谱（显示出了铁相对氧与硅的高度集中）令人信服地说明，抛出的物质是爆发白矮星的残余。遗迹的大小和温度说明，它有着几千年的历史。

Astronomers have identified two major types of supernovas: Type II, in which a massive star explodes; and Type Ia, in which a white dwarf star explodes because it has pulled too much material from a nearby companion star onto itself. 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. This was the case in DEM L71.

天文学家主要将超新星划分为两大类：II型，也就是大质量恒星的爆发；还有Ia型，也就是吸积过多邻近伴星物质的白矮星发生的爆炸。如果白矮星的质量超过了太阳的1.4倍，它会变得不稳定，并在热核爆炸中碎裂。这就是DEM L71的情况。

One of the major goals of the study of supernova remnants is to determine the type of supernova explosion. The identification of DEM L71 as the remnant of an exploded white dwarf, or Type Ia supernova, represents a major step forward in understanding more about the ways in which stars explode.

研究超新星遗迹的一大目标是确定超新星爆发的种类。将DEM L71辨认为白矮星爆发（或说Ia型超新星）的产物，标志着又在了解恒星爆发方式的道路上前进了一大步。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 18:22 编辑 ]

N132D:
Glowing Remnant from a Star-Shattering Explosion


N132D：恒星爆炸产生的光辉遗迹

This "true color" Chandra image of N132D shows the beautiful, complex remnant of an explosion of a massive star in the Large Magellanic Cloud, a nearby galaxy about 160,000 light years from Earth. The colors represent different ranges of X-rays, with red, green, and blue representing, low, medium, and higher X-ray energies respectively.

这张钱德拉拍摄的N132D“真彩色图象”展现了一个漂亮而复杂的遗迹，它产生于160000光年外的邻近星系——大麦哲伦云中某颗大质量恒星的爆发。颜色代表不同的X射线波段，红、绿、蓝色分别表示低、中、高能X射线。

Supernova remnants comprise debris of a stellar explosion and any matter in the vicinity that is affected by the expanding debris. In the case of N132D, the horseshoe shape of the remnant is thought to be due to shock waves from the collision of the supernova ejecta with cool giant gas clouds. As the shock waves move through the gas they heat it to millions of degrees, producing the glowing X-ray shell.

超新星遗迹由恒星爆发产生的碎片与附近被膨胀残骸扰动过的一切物质组成。在N132D中，遗迹的马蹄铁状外观据信是因超新星抛出物与巨大的冷分子云相撞所致的。激波扫过气体时，它们会将气体加热到上百万度，产生发光的X射线壳层。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 18:23 编辑 ]

漂亮的一塌糊涂啊。

N63A:
Celestial Illumination: The X-Ray Glow From An Exploded Star

来源: http://chandra.harvard.edu/photo/2003/n63a/index.html

N63A：
照彻天宇：爆发超新星的X射线辉光

Chandra has imaged the glowing shell created by the destruction of a massive star. X-rays from Chandra (blue), combined with optical (green) and radio (red) data, reveal new details in the supernova remnant known as N63A, located in the nearby galaxy of the Large Magellanic Cloud.

钱德拉拍摄下了大质量恒星的摧毁产生的明亮壳层。来自钱德拉的X射线数据（蓝色）结合可见光（绿色）与射电（红色）数据，一道揭示了超新星遗迹N63A的新细节。N63A位于邻近星系大麦哲伦云中。

The X-ray glow is from material heated to about ten million degrees Celsius by a shock wave generated by the supernova explosion. The age of the remnant is estimated to be in the range of 2,000 to 5,000 years.

被超新星爆发的激波加热到1000万摄氏度的物质发出了X射线辐射。推知的遗迹年龄在2000年到5000年之间。

Optical and radio light are brightest in the central region of the remnant, which appears as a triangular-shaped "hole" in the X-ray image. The hole is produced by absorption of X-rays in a dense cloud of cooler gas and dust on the side of the remnant nearest the Earth. A comparison of the X-ray image with the radio and optical images suggests that the shock wave is engulfing this massive cloud, so we see only the edge nearest the Earth. Collisions such as this are thought to trigger the formation of new generations of stars.

遗迹中央的可见光和射电辐射最为明亮，这里在X射线照片上呈三角形的“洞穴”状。洞穴的成因是遗迹靠近地球的一侧有着致密的冷气体/尘埃云团吸收X射线。通过比较X射线、射电和可见光图象可以得知，激波吞没了巨大的云团，因此我们只能看到其靠近地球一侧的边缘区域。据信这样的撞击过程会触发新一代恒星的形成。

The fluffy crescent-shaped X-ray features that appear around the edge of the remnant are thought to be fragments of high-speed matter shot out from the star when it exploded, like shrapnel from a bomb. In the only other supernova remnant (the Vela supernova remnant) where such features have been observed, the crescent shapes are clearly produced by ejecta fragments. An alternative explanation is that they were produced when the shock wave swept over less-massive clouds located several light years away from the site of the explosion.

X射线下，环绕遗迹边缘的蓬松新月状结构据信是恒星爆发时高速抛出的物质的残留，类似于炸弹的弹片。其他超新星遗迹中，只有一个（船帆座超新星遗迹）观测到了这样的特征，可以确信，该遗迹的新月形外观是抛出的碎片造就的。另一种解释是，是扫过爆发点几光年之外的小质量云团的激波造就了这样的特征。

                               
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Inverted Chandra X-ray Image of N63A

N63A的钱德拉X射线反向照片
Chandra's image of N63A shows material heated to about ten million degrees Celsius by a shock wave generated by the supernova explosion. This image has been inverted to better show the fluffy crescent-shaped X-ray features that appear around the edge of the remnant. The features are thought to be fragments of high-speed matter shot out from the star when it exploded, like shrapnel from a bomb.
Scale: Image is 112 arcsec per side



钱德拉的N63A照片展现了被超新星爆发的激波加热到1000万摄氏度的物质。为更好地展现遗迹边缘蓬松的新月状结构，图片已被翻转。这样的特征信是恒星爆发时高速抛出的物质的残留，类似于炸弹的弹片。

                               
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Chandra X-ray Image of N63A
Chandra's image of N63A shows material heated to about ten million degrees Celsius by a shock wave generated by the supernova explosion. The fluffy crescent-shaped X-ray features that appear around the edge of the remnant are thought to be fragments of high-speed matter shot out from the star when it exploded, like shrapnel from a bomb.
Scale: Image is 112 arcsec per side
(Credit: NASA/CXC/Rutgers/J.Warren et al.)



钱德拉拍摄的N63A X射线照片
钱德拉的N63A照片展现了被超新星爆发的激波加热到1000万摄氏度的物质。环绕遗迹边缘的蓬松新月状结构据信是恒星爆发时高速抛出的物质的残留，类似于炸弹的弹片。
比例：图象边长对应112角秒
版权：NASA/CXC/Rutgers/J.Warren et al.

                               
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Chandra 3-Color X-ray Image of N63A
Chandra's image of N63A shows material heated to about ten million degrees Celsius by a shock wave generated by the supernova explosion. The fluffy crescent-shaped X-ray features that appear around the edge of the remnant are thought to be fragments of high-speed matter shot out from the star when it exploded, like shrapnel from a bomb. The colors red, green and blue in the image correspond to low, medium and high-energy X-rays, respectively.
Scale: Image is 112 arcsec per side
(Credit: NASA/CXC/Rutgers/J.Warren et al.)

钱德拉拍摄的N63A三色X射线图
钱德拉的N63A照片展现了被超新星爆发的激波加热到1000万摄氏度的物质。环绕遗迹边缘的蓬松新月状结构据信是恒星爆发时高速抛出的物质的残留，类似于炸弹的弹片。红、绿、蓝色各代表低能、中能和高能X射线。
比例：图象边长对应112角秒
版权：NASA/CXC/Rutgers/J.Warren et al.

                               
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HST Optical Image of N63A
This visible-light image of supernova remnant N63A was taken by the Hubble Space Telescope's Wide Field and Planetary Camera 2 (WFPC2) on August 10, 1997. The optical light is brightest in the central region of the remnant, which appears as a triangular-shaped "hole" in the X-ray data. The field of view is the same as the Chandra image.
Scale: Image is 112 arcsec per side
(Credit: NASA/STScI/U. Ill/Y.Chu)



哈勃拍摄的N63A光学图象
超新星遗迹N63A的光学图象由哈勃太空望远镜宽视场和行星照相机II（WFPC2）于1997年8月10日拍摄。遗迹的中心区域在可见光下很明亮，而这里在X射线数据中则呈三角形的“洞穴”。视场与钱德拉的图象相同。
比例：图象边长对应112角秒
版权：NASA/STScI/U. Ill/Y.Chu

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 11:55 编辑 ]

Cassiopeia A:
Chandra's Celestial Fireworks

来源:http://chandra.harvard.edu/photo/2002/0237/index.html

仙后座A：钱德拉的宇宙焰火

In August of 1999, NASA released an image of Cassiopeia A, a supernova remnant revealed in never-before-seen X-ray detail. The "Cas A" image, as it has come to be known, shows remarkable structure in the debris of a gigantic stellar explosion, as well as an enigmatic source in the center, which could be a rapidly spinning neutron star or black hole. The Chandra X-ray Observatory image of Cas A ushered in a new era of X-ray astronomy. This image was produced from the archives to celebrate the anniversary of Chandra’s first light. The low, medium, and higher X-ray energies of the Chandra data are shown as red, green, and blue respectively.

1999年8月，NASA公布了仙后座A的照片。这是一个超新星遗迹，照片揭示出了前所未有的X射线细节。这张业已为人所知的Cas A照片展现了产生于剧烈恒星爆发的碎片那非凡的结构，此外还有中心的神秘辐射源，它可能是个快速旋转的中子星或黑洞。钱德拉X射线天文台拍摄的Cas A图象引领了X射线天文学的新时代。该图是为庆祝钱德拉的首次飞行周年纪念而利用档案数据制作的。钱德拉数据中的低、中、高能X射线分别以红、绿、蓝色表示。

                               
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Cassiopeia A in Many Colors

来源:http://chandra.harvard.edu/photo/2005/casa/index.html

多色仙后座A

This stunning picture of the supernova remnant Cassiopeia A (Cas A) is a composite of images taken by three of NASA's Great Observatories. Infrared data from the Spitzer Space Telescope are colored red; optical data from the Hubble Space Telescope are yellow; and X-ray data from the Chandra X-ray Observatory are green and blue.

仙后座A超新星遗迹（Cas A）的震撼图象是NASA的三架大天文台照片的合成。来自斯必泽太空望远镜的红外数据以红色表示，哈勃太空望远镜的可见光数据用黄色表示，而钱德拉X射线天文台的X射线数据用绿色和蓝色表示。

Cas A is the 300-year-old remnant created by the supernova explosion of a massive star. Each Great Observatory image highlights different characteristics of the remnant. Spitzer reveals warm dust in the outer shell with temperatures of about 10 degrees Celsius (50 degrees Fahrenheit), and Hubble sees the delicate filamentary structures of warmer gases about 10,000 degrees Celsius. Chandra shows hot gases at about 10 million degrees Celsius. This hot gas was created when ejected material from the supernova smashed into surrounding gas and dust at speeds of about ten million miles per hour.

仙后座A是有着300年历史的遗迹，成因是大质量恒星的超新星爆发。各天文台的图象突出了遗迹不同的特点。斯必泽揭示的是外壳层中温热的尘埃，温度大约是10摄氏度（50华氏度），哈勃所见的主要是精细的纤维结构，由温度更高（10000摄氏度）的气体组成。钱德拉展现的是约莫1000万摄氏度高温的热气体。热气体的成因是，超新星抛出的物质以每小时1000万英里的速度冲入周围气体和尘埃。

A comparison of the infrared and X-ray images of Cas A should enable astronomers to better understand how relatively cool dust grains can coexist in the superhot gas that produces the X-rays. It should also help to determine whether most of the dust in the supernova remnant came from the massive star before it exploded, or from the rapidly expanding supernova ejecta.

比较Cas A的红外与X射线图片，天文学家可以更好地了解相对较冷的颗粒如何与产生X射线的热气体共生。这还可以帮助人们确定，超新星遗迹中的大部分尘埃究竟源于爆发前的大质量恒星，还是来自迅速膨胀的超新星抛出物。

The turquoise dot at the center of the shell may be a neutron star created during the supernova. Blue Chandra data were acquired using broadband X-rays (low through high energies); green Chandra data correspond only to intermediate energy X-rays; yellow Hubble data were taken using a 900 nanometer-wavelength filter, and red Spitzer data are from the telescope's 24-micron detector.

壳层中心处的青色光点可能是超新星造就的中子星。钱德拉数据中的蓝色部分是使用宽带X射线（低能至高能）得到的，而绿色部分只代表中能X射线。以黄色表示的哈勃数据使用900纳米波长的滤镜拍摄，而以红色表示的斯必泽数据是用望远镜的24微米探测器测出的。

                               
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未完待续

难得的好贴子！！！！！！！！！！

Cassiopeia A:
Deepest Image of Exploded Star Uncovers Bipolar Jets

来源:http://chandra.harvard.edu/photo/2004/casa/index.html

仙后座A：爆发恒星的深度图片揭示出了双极喷流

This spectacular image of the supernova remnant Cassiopeia A is the most detailed image ever made of the remains of an exploded star. 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. A large jet-like structure that protrudes beyond the shock wave can be seen in the upper left. In the accompanying image, specially processed to highlight silicon ions, a counter-jet can be seen on the lower right.

这张壮观的仙后座A照片是迄今对爆发恒星的残骸拍摄过的最精细的照片。曝光100万秒的图象揭示出了直径10光年的明亮外环（绿色），这里标志着超新星爆发产生的激波起源。左上可见突出激波的庞大喷流结构。附随的照片特别加亮了硅离子，其右下可见反向喷流。

Surprisingly, the X-ray spectra show that the jet and counter-jet are rich in silicon atoms and relatively poor in iron atoms. This indicates that the jets formed soon after the initial explosion of the star; otherwise, the jets should have contained large quantities of iron from the star's central regions
奇怪的是，X射线光谱表明，喷流与反向喷流富含硅原子，但铁原子丰度较小。这说明，喷流在初始的恒星爆发之后很快形成。否则，喷流中将含有大量来自恒星中心的铁。

The bright blue fingers located near the shock wave on the lower left are composed almost purely of iron gas. This iron was produced in the central, hottest regions of the star and somehow ejected in a direction almost perpendicular to the jets.

激波附近，明亮的蓝色指状物（左下）几乎全由铁原子气组成。铁产生于恒星中央最炽热的区域里，被某种机制以垂直于喷流的方向抛了出去。

The bright source at the center of the image is presumed to be a neutron star created during the supernova. Unlike the rapidly rotating neutron stars in the Crab Nebula and Vela supernova remnants that are surrounded by dynamic magnetized clouds of electrons called pulsar wind nebulas, this neutron star is quiet, faint, and so far shows no evidence for pulsed radiation.

图片中心的明亮辐射源据信是超新星爆发过程中产生的中子星。与蟹状星云和船帆座超新星遗迹中被磁化电子云（脉冲星风星云）环绕的高速自转中子星不同，这颗中子星安静而虚弱，目前为止，没有显示脉冲辐射的迹象。

A working hypothesis is that the explosion that created Cassiopeia A produced high-speed jets similar to but less energetic than the hypernova jets thought to produce gamma-ray bursts. During the explosion, the neutron star may have developed an extremely strong magnetic field that helped to accelerate the jets. This strong magnetic field later stifled any pulsar wind activity, so the neutron star today resembles other strong-field neutron stars (a.k.a. "magnetars") in lacking a pulsar wind nebula.

通行的假设是，产生仙后座A的爆发产生的高速喷流类似于产生伽玛射线暴的超超新星（hypernova），不过没有那么高的能量。爆发过程中，中子星可能产生了促进喷流加速的超强磁场。稍后，强磁场抑制了一切脉冲星风的活动，因此今天的中子星在缺乏星风这一点上，类似其他强磁场中子星（即磁星）。

                               
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Kepler's Supernova Remnant:
NASA's Great Observatories Provide a Detailed View of Kepler's Supernova Remnant



开普勒超新星遗迹：NASA大天文台眼中的开普勒超新星遗迹细节
来源:http://chandra.harvard.edu/photo/2004/kepler/index.html

NASA's three Great Observatories -- the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory -- joined forces to probe the expanding remains of a supernova. Now known as Kepler's supernova remnant, this object was first seen 400 years ago by sky watchers, including famous astronomer Johannes Kepler.

NASA的三架大天文台，也就是哈勃太空望远镜、斯必泽太空望远镜以及钱德拉X射线天文台联合起来，探测着膨胀的超新星遗迹。这个名为开普勒超新星遗迹的天体是400年前的观测者所发现的，其中就包括著名天文学家约翰尼斯·开普勒。

The combined image unveils a bubble-shaped shroud of gas and dust that is 14 light years wide and is expanding at 4 million miles per hour (2,000 kilometers per second). Observations from each telescope highlight distinct features of the supernova remnant, a fast-moving shell of iron-rich material from the exploded star, surrounded by an expanding shock wave that is sweeping up interstellar gas and dust.

合成图揭示了气体和尘埃组成的泡状覆盖物，宽14光年，以每秒400万英里（每秒2000公里）的速度膨胀。各望远镜的观测突出的是超新星遗迹不同的部位，恒星爆发产生的高速富铁壳层，周围包裹着膨胀的激波，扫过星际气体和尘埃。

Each color in this image represents a different region of the electromagnetic spectrum, from X-rays to infrared light. These diverse colors are shown in the panel of photographs below the composite image. The X-ray and infrared data cannot be seen with the human eye. By color-coding those data and combining them with Hubble's visible-light view, astronomers are presenting a more complete picture of the supernova remnant.

图中，每种颜色代表从红外到X射线的不同电磁波波段。不同的色彩在合成图下方的小图中分别表示。肉眼不能看到X射线和红外。将其按一定的规则着色，再结合哈勃的可见光图象，天文学家呈献出的是超新星遗迹更完整的图象。

Visible-light images from the Hubble telescope (colored yellow) reveal where the supernova shock wave is slamming into the densest regions of surrounding gas.

哈勃望远镜拍摄的可见光照片（以黄色表示）揭示出的是超新星的激波，正冲入周边最致密的气体中。

The bright glowing knots are dense clumps from instabilities that form behind the shock wave. The Hubble data also show thin filaments of gas that look like rippled sheets seen edge-on. These filaments reveal where the shock wave is encountering lower-density, more uniform interstellar material.

发光的亮结是致密的云团块，源自激波后方的不稳定性。哈勃的数据还展现了纤细的气体纤维，看起来象是侧面所见的波纹板。纤维揭示的是激波与更均匀的低密度星际物质相遇的地方。

The Spitzer telescope shows microscopic dust particles (colored red) that have been heated by the supernova shock wave. The dust re-radiates the shock wave's energy as infrared light. The Spitzer data are brightest in the regions surrounding those seen in detail by the Hubble telescope.

斯必泽望远镜的数据展现了超新星激波加热过的微观尘埃颗粒（以红色表示）。尘埃在红外波段重新发射着激波的能量。斯必泽的数据中，最明亮的部分包围着哈勃所见的细节。

The Chandra X-ray data show regions of very hot gas, and extremely high energy particles.

钱德拉的X射线数据表现的是极高温的气体以及极高能宇宙线。

The hottest gas (higher-energy X-rays, colored blue) is located primarily in the regions directly behind the shock front. These regions also show up in the Hubble observations, and also align with the faint rim of glowing material seen in the Spitzer data. The X-rays from the region on the lower left (blue) may be dominated by extremely high energy electrons that were produced by the shock wave and are radiating at radio through X-ray wavelengths as they spiral in the intensified magnetic field behind the shock front. Cooler X-ray gas (lower-energy X-rays, colored green) resides in a thick interior shell and marks the location of heated material expelled from the exploded star.

最热的气体（高能X射线，以蓝色表示）主要位于激波波前的后方。这些区域见于哈勃的观测中，也与斯必泽所见的发光物质暗边吻合。来自左下方的X射线（蓝色）可能是极高能电子占据主导的，它们是激波的产物，当它们沿螺旋线落向激波波前后方的加强磁场时，在从射电到X射线的波段上发出辐射。温度较低的X射线气体（低能X射线，以绿色表示）位于厚厚的内壳层中，标志着爆发恒星抛射加热物质的方位。

The remnant of Kepler's supernova, the last such object seen to explode in our Milky Way galaxy (with the possible exception of the Cassiopeia A supernova, for which ambiguous sightings were reported around 1680), is located about 13,000 light years away in the constellation Ophiuchus.

开普勒超新星遗迹是银河系中爆发的最近的一颗超新星遗迹（也许仙后座A的前身超新星是个例外，有1680年左右不明确的目击记录留存。），距离我们13000光年，位于蛇夫座。

                               
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Kepler's Supernova Remnant:

开普勒超新星遗迹：

X-射线，光学和红外综合

                               
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X-射线(高能源)

                               
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X-射线(低能源)

                               
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光学

                               
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红外线

                               
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怎么会有如此绚丽的色彩啊…………

精妙绝伦。
宇宙的神奇。

色彩非常不错。。。。