ASTRO-114--Lecture 38-
... and look up at the stars. And after a little practice, they could pick a star and tell what its magnitude was. Because you only had six numbers to choose from and usually you could tell whether it was first, ‘cause they were very bright, or whether it was sixth, because you could hardly see them, an ...
... and look up at the stars. And after a little practice, they could pick a star and tell what its magnitude was. Because you only had six numbers to choose from and usually you could tell whether it was first, ‘cause they were very bright, or whether it was sixth, because you could hardly see them, an ...
Pp 263-266 - Gravity From The Ground Up
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
Document
... surface temperature (with the same radius) are brighter (StephanBoltzmann Law), so they must move up to the left. Stars of the same surface temperature, that are brighter, must be larger stars. Oct 31, 2003 ...
... surface temperature (with the same radius) are brighter (StephanBoltzmann Law), so they must move up to the left. Stars of the same surface temperature, that are brighter, must be larger stars. Oct 31, 2003 ...
Slide
... Parallax Measurements • Earth-based measurements can typically be made to 0.03”, or to a distance of ~30 parsecs (pc) • Distances to several thousand stars are known this way. • The Hipparcos satellite extends the distance to ~200 pc, so distances to nearly one million stars can be measured with pa ...
... Parallax Measurements • Earth-based measurements can typically be made to 0.03”, or to a distance of ~30 parsecs (pc) • Distances to several thousand stars are known this way. • The Hipparcos satellite extends the distance to ~200 pc, so distances to nearly one million stars can be measured with pa ...
DTU_9e_ch15
... stars in the vicinity of the unseen massive object () at the position of the radio source Sagittarius A*, part of Sgr A. This plot indicates that the stars are held in orbit by a 4 x 106solar-mass black hole. ...
... stars in the vicinity of the unseen massive object () at the position of the radio source Sagittarius A*, part of Sgr A. This plot indicates that the stars are held in orbit by a 4 x 106solar-mass black hole. ...
The Formation of Massive Star Systems by Accretion
... and the resulting formation of companion stars (11) can only be simulated when the disk is represented nonaxisymmetrically. It is important to consider these effects because most massive stars are members of multiple systems (12, 13). Our initial conditions consisted of a gas cloud with mass = 100 M ...
... and the resulting formation of companion stars (11) can only be simulated when the disk is represented nonaxisymmetrically. It is important to consider these effects because most massive stars are members of multiple systems (12, 13). Our initial conditions consisted of a gas cloud with mass = 100 M ...
Variable Stars – II. Pulsating stars
... Cepheids are variable supergiant stars with similar temperatures to the Sun. They are named after the prototype δ Cephei and are also called δ Cepheids or type I Cepheids, for reasons which will become evident. The first recorded discovery of the variation in δ Cephei was by John Goodricke in 1784. ...
... Cepheids are variable supergiant stars with similar temperatures to the Sun. They are named after the prototype δ Cephei and are also called δ Cepheids or type I Cepheids, for reasons which will become evident. The first recorded discovery of the variation in δ Cephei was by John Goodricke in 1784. ...
Asteroseismology of Solar-Like Stars
... observationally present within more evolved, or more massive, stars than that of the Sun. In pressure modes the restoring force is the pressure gradient within the star. p modes are the acoustic waves excited by the stochastic turbulence of the near-surface convection zones. These acoustic oscillati ...
... observationally present within more evolved, or more massive, stars than that of the Sun. In pressure modes the restoring force is the pressure gradient within the star. p modes are the acoustic waves excited by the stochastic turbulence of the near-surface convection zones. These acoustic oscillati ...
Chandra Observation of Pulsar Wind Nebula
... We find intriguing spectral hardening in regions of the radio and X-ray shell, which can only be explained by the new particle acceleration. This shows that the pulsar wind bubble can expand supersonically and generate shocks, even in such an old (5×105 yr) system. The optical filaments are also pr ...
... We find intriguing spectral hardening in regions of the radio and X-ray shell, which can only be explained by the new particle acceleration. This shows that the pulsar wind bubble can expand supersonically and generate shocks, even in such an old (5×105 yr) system. The optical filaments are also pr ...
Science and the Universe
... size that orbits a star and does not produce its own light • A star is large body which (at some point during its life) produces light by nuclear reactions ...
... size that orbits a star and does not produce its own light • A star is large body which (at some point during its life) produces light by nuclear reactions ...
Chapter14(4-7-11)
... • 14.1 The Milky Way Revealed • 14.2 Galactic Recycling (closely related to Ch. 13) • 14.3 The History of the Milky Way • 14.4 The Mysterious Galactic Center ...
... • 14.1 The Milky Way Revealed • 14.2 Galactic Recycling (closely related to Ch. 13) • 14.3 The History of the Milky Way • 14.4 The Mysterious Galactic Center ...
WORD - Astrophysics
... (probably crucial) role in determining the morphological type of a given galaxy, but we do not know what merged, or when it merged -- how do the merging histories of non-baryonic dark matter and of baryons compare? Similarly, stars clearly form(ed) at some rate from gas, but at what rate, where, wit ...
... (probably crucial) role in determining the morphological type of a given galaxy, but we do not know what merged, or when it merged -- how do the merging histories of non-baryonic dark matter and of baryons compare? Similarly, stars clearly form(ed) at some rate from gas, but at what rate, where, wit ...
Feb 2015 - Bluewater Astronomical Society
... Outburst from Milky Way’s Black Hole Astronomers have observed the largest X-ray flare ever detected from the supermassive black hole at the center of the Milky Way galaxy. This event, detected by NASA’s Chandra X-ray Observatory, raises questions about the behavior of this giant black hole and its ...
... Outburst from Milky Way’s Black Hole Astronomers have observed the largest X-ray flare ever detected from the supermassive black hole at the center of the Milky Way galaxy. This event, detected by NASA’s Chandra X-ray Observatory, raises questions about the behavior of this giant black hole and its ...
3D maps of the local interstellar medium: searching for the imprints
... impact of a massive external cloud or a series of explosive events, potentially initiated by a major one, such as a GRB. The former scenario naturally explains the inclination, while the latter is better in that it accounts for the expanding and rotating belt. Developing further the collision scenar ...
... impact of a massive external cloud or a series of explosive events, potentially initiated by a major one, such as a GRB. The former scenario naturally explains the inclination, while the latter is better in that it accounts for the expanding and rotating belt. Developing further the collision scenar ...
Table of Contents - Shawnee State University
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
ASTRO-114--Lecture 37-
... background behind an object you’re looking at and so you can tell how far away an object is by how much parallax you see with it from one eye to the other. In other words, looking at your thumb, shifting from one eye to the other, you see a shift. You can then tell your thumb is fairly close. Now, l ...
... background behind an object you’re looking at and so you can tell how far away an object is by how much parallax you see with it from one eye to the other. In other words, looking at your thumb, shifting from one eye to the other, you see a shift. You can then tell your thumb is fairly close. Now, l ...
Star Formation in Bok Globules - European Southern Observatory
... CG 1 is not the only one of the globules in the Gum Nebula wh ich has formed stars, several of them are associated with stars and Herbig-Haro objects. Herbig-Haro objects are small nebulosities with peculiar forbidden emission-li ne spectra found in certain star-forming dark clouds. Often these obje ...
... CG 1 is not the only one of the globules in the Gum Nebula wh ich has formed stars, several of them are associated with stars and Herbig-Haro objects. Herbig-Haro objects are small nebulosities with peculiar forbidden emission-li ne spectra found in certain star-forming dark clouds. Often these obje ...
A near IR adaptive optics search for faint companions to early
... show a new bright component P (K = 11.2) and at least two additional fainter components Q and R. While little can be said about the fainter sources, the P component is very likely physical, judging by its proximity to C and its brightness. Its colour J − K = 1.24 is too red for a normal star, but no ...
... show a new bright component P (K = 11.2) and at least two additional fainter components Q and R. While little can be said about the fainter sources, the P component is very likely physical, judging by its proximity to C and its brightness. Its colour J − K = 1.24 is too red for a normal star, but no ...
PH607lec12-5gal3
... fainter lines in this region due to [NII]. HII regions appear reddish in this image because of the prominence of the H alpha line in the red region of the spectrum. The dark features running vertically trace emission in the hydrogen H-alpha line (left and stronger feature, rest wavelength 6563 Angst ...
... fainter lines in this region due to [NII]. HII regions appear reddish in this image because of the prominence of the H alpha line in the red region of the spectrum. The dark features running vertically trace emission in the hydrogen H-alpha line (left and stronger feature, rest wavelength 6563 Angst ...
MAIN SEQUENCE STARS, Red Giants and White Dwarfs
... He BURNING MAIN SEQUENCE -- which is visible on an H-R diagram as the HORIZONTAL BRANCH (lower L but higher Ts than during the He flash). o Stars are again in HYDROSTATIC EQUILIBRIUM throughout: the thermostat works again o These are still RGs, and on HB the higher masses are to the left part of the ...
... He BURNING MAIN SEQUENCE -- which is visible on an H-R diagram as the HORIZONTAL BRANCH (lower L but higher Ts than during the He flash). o Stars are again in HYDROSTATIC EQUILIBRIUM throughout: the thermostat works again o These are still RGs, and on HB the higher masses are to the left part of the ...
Physics of Star Formation: Milky Way and Beyond
... this structure affect their production of stars? This paper presents new models of axisymmetric star-forming filaments having no cores, one low-mass core, and one cluster-forming core. The models resemble observed clouds in their column density maps and radial profiles, and their N-pdf distributions ...
... this structure affect their production of stars? This paper presents new models of axisymmetric star-forming filaments having no cores, one low-mass core, and one cluster-forming core. The models resemble observed clouds in their column density maps and radial profiles, and their N-pdf distributions ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... starburst galaxies. After amassing a reasonable amount of galaxies (about 70), we calculated the ratios between the prominent emission lines. To find these ratios we divided the higher wavelength by the shorter one. We had to find the ratios of all the emission lines in order to discover which eleme ...
... starburst galaxies. After amassing a reasonable amount of galaxies (about 70), we calculated the ratios between the prominent emission lines. To find these ratios we divided the higher wavelength by the shorter one. We had to find the ratios of all the emission lines in order to discover which eleme ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.