Physics-Y11-LP3 - All Saints` Catholic High School
... • understand the role of observations of Cepheid variable stars in establishing the scale of the Universe and the nature of most spiral nebulas as distant galaxies • describe some of the new information that telescopes revealed about the Milky Way and objects beyond the Milky Way • recall the main i ...
... • understand the role of observations of Cepheid variable stars in establishing the scale of the Universe and the nature of most spiral nebulas as distant galaxies • describe some of the new information that telescopes revealed about the Milky Way and objects beyond the Milky Way • recall the main i ...
File
... • are recent discovery (by Edwin Hubble in late 1920’s) • can be classified by morphology (shapes and sizes) Three Main Types of Galaxies: • Ellipticals - galaxies are pure bulge, no disk component ...
... • are recent discovery (by Edwin Hubble in late 1920’s) • can be classified by morphology (shapes and sizes) Three Main Types of Galaxies: • Ellipticals - galaxies are pure bulge, no disk component ...
Multiwavelength Astronomy: Your World in Different Lights
... Right now, every object in the room around you is emitting electromagnetic waves…your shoes, your chair, the wall, even you…Everything is radiating! Anything with any heat energy whatsoever radiates electromagnetic waves. The only way an object could not emit radiation is if its temperature were abs ...
... Right now, every object in the room around you is emitting electromagnetic waves…your shoes, your chair, the wall, even you…Everything is radiating! Anything with any heat energy whatsoever radiates electromagnetic waves. The only way an object could not emit radiation is if its temperature were abs ...
h-r_diagram_online_lab
... astronomer Henry Norris Russell created a diagram of stars plotted using only their luminosity and their spectral types. A star’s spectral type is determined by the absorption lines found in its spectrum. Hertzsprung and Russell noticed that the spectra were related to the stars’ color and temperatu ...
... astronomer Henry Norris Russell created a diagram of stars plotted using only their luminosity and their spectral types. A star’s spectral type is determined by the absorption lines found in its spectrum. Hertzsprung and Russell noticed that the spectra were related to the stars’ color and temperatu ...
Transcript - Chandra X
... All stars are ~75% hydrogen, ~ 24% helium, and ~1% metals. There are more than 150 globulars in the MWG. There is less gas, and the older stars are towards the center with younger stars gravitating towards the ended. The orbits of globular clusters can take them through the plane of the galaxy which ...
... All stars are ~75% hydrogen, ~ 24% helium, and ~1% metals. There are more than 150 globulars in the MWG. There is less gas, and the older stars are towards the center with younger stars gravitating towards the ended. The orbits of globular clusters can take them through the plane of the galaxy which ...
Looking out at the Night Sky What questions do you have?
... in Rio de Janiero? When it is low in our sky, where is it in Rio? ...
... in Rio de Janiero? When it is low in our sky, where is it in Rio? ...
Astro 204: Practice Questions Some of these questions are a bit
... 19. A bright star is observed to orbit a supermassive black hole in a circular orbit with a period of 20 years. The orbital plane is inclined with respect to the plane of the sky by 30◦ . Observations of various lines in the stellar spectrum show that the maximum line-of-sight velocity exhibited by ...
... 19. A bright star is observed to orbit a supermassive black hole in a circular orbit with a period of 20 years. The orbital plane is inclined with respect to the plane of the sky by 30◦ . Observations of various lines in the stellar spectrum show that the maximum line-of-sight velocity exhibited by ...
Nuclear fusion in stars and laboratories
... ² We have thus been led to the following view of stellar evolution. 1. Stars form by collapse of interstellar gas clouds under the in°uence of gravity. As they shrink, they release gravitational energy. Once a protostar has become su±ciently dense to be opaque, this energy cannot be freely radiated ...
... ² We have thus been led to the following view of stellar evolution. 1. Stars form by collapse of interstellar gas clouds under the in°uence of gravity. As they shrink, they release gravitational energy. Once a protostar has become su±ciently dense to be opaque, this energy cannot be freely radiated ...
April
... Galaxy for it’s elongated shape, M82 is also about 12 million Light Years distant. The close encounter with M81 described above distorted the shape of this irregular galaxy, creating considerable turbulence in its innermost regions. Over 100 globular clusters have been observed orbiting this galaxy. ...
... Galaxy for it’s elongated shape, M82 is also about 12 million Light Years distant. The close encounter with M81 described above distorted the shape of this irregular galaxy, creating considerable turbulence in its innermost regions. Over 100 globular clusters have been observed orbiting this galaxy. ...
Linking Asteroids and Meteorites through Reflectance
... • At the dawn of the 20th century, most astronomers thought that the Milky Way Galaxy was the universe, and it measured only a few thousand light-years across. ...
... • At the dawn of the 20th century, most astronomers thought that the Milky Way Galaxy was the universe, and it measured only a few thousand light-years across. ...
First firm spectral classification of an early-B pre-main
... that the star is not leaving the main sequence before the accretion process has finished. Evidence of accretion must come from the detection of circumstellar disks, and possibly bipolar jets, as observed around forming low-mass stars (e.g., Appenzeller & Mundt 1989). Disks and outflows around massiv ...
... that the star is not leaving the main sequence before the accretion process has finished. Evidence of accretion must come from the detection of circumstellar disks, and possibly bipolar jets, as observed around forming low-mass stars (e.g., Appenzeller & Mundt 1989). Disks and outflows around massiv ...
Central Temperature and Density of Stars in Gravitational Equilibrium
... to hold between the pressure and density throughout the whole interior. Secondly, for a star having a shell structure our consideration is confined to its innermost homogeneous core. The pressure at the core boundary is assumed to be so small compared to the central pressure that the existence of th ...
... to hold between the pressure and density throughout the whole interior. Secondly, for a star having a shell structure our consideration is confined to its innermost homogeneous core. The pressure at the core boundary is assumed to be so small compared to the central pressure that the existence of th ...
l`Astrofilo - Astro Publishing
... The possibilities become more interesting for the wide binary M-G star scenarios. The primary star's radiation always has a greater magnitude than that of the distant secondary star; however, there are periods where a portion of the planet would be illuminated only by light from the less photosynthe ...
... The possibilities become more interesting for the wide binary M-G star scenarios. The primary star's radiation always has a greater magnitude than that of the distant secondary star; however, there are periods where a portion of the planet would be illuminated only by light from the less photosynthe ...
Scientific requirements of ALMA, and its capabilities for key
... LSB: H13CN 4-3, CS 7-6, CO 3-2 SCUBA 450 micron ...
... LSB: H13CN 4-3, CS 7-6, CO 3-2 SCUBA 450 micron ...
Rotation
... and the Eddington Sweet time scale is about 1012 years, i.e., it is unimportant. It can become more important near the surface though as the density decreases (Kippenhahn 42.36) For a 20 M e star , the Kelvin Helmholtz time scale relative to the nuclear lifetime is about three times greater . More i ...
... and the Eddington Sweet time scale is about 1012 years, i.e., it is unimportant. It can become more important near the surface though as the density decreases (Kippenhahn 42.36) For a 20 M e star , the Kelvin Helmholtz time scale relative to the nuclear lifetime is about three times greater . More i ...
April 2005
... • Too distant to resolve the individual stars • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their spectral lines ...
... • Too distant to resolve the individual stars • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their spectral lines ...
Review 3 (11-18-10)
... stars we born at the same time, we can measure a cluster’s age by finding the main sequence turnoff point on an H–R diagram of its stars. The cluster’s age is equal to the hydrogenburning lifetime of the hottest, most luminous stars that remain on the main sequence. ...
... stars we born at the same time, we can measure a cluster’s age by finding the main sequence turnoff point on an H–R diagram of its stars. The cluster’s age is equal to the hydrogenburning lifetime of the hottest, most luminous stars that remain on the main sequence. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.