galaxy.
... our galaxy for several reasons • Galaxy was huge (he didn’t know about dust). • van Maanen’s observations showed that one spiral nebula, M 101, could be observed to rotate. It it were outside our galaxy, it would have to be turning faster than the speed of light. • Spiral nebulae were never seen in ...
... our galaxy for several reasons • Galaxy was huge (he didn’t know about dust). • van Maanen’s observations showed that one spiral nebula, M 101, could be observed to rotate. It it were outside our galaxy, it would have to be turning faster than the speed of light. • Spiral nebulae were never seen in ...
SMMP_BISANA - Infinity and Beyond
... Despite the many mentions of the stars in Greek and early Roman texts, by far the most thorough star catalogue from ancient times belongs to the Roman Ptolemy of Alexandria, who grouped 1022 stars into 48 constellations during the 2nd century A.D. Although Ptolemy's Almagest does not include the co ...
... Despite the many mentions of the stars in Greek and early Roman texts, by far the most thorough star catalogue from ancient times belongs to the Roman Ptolemy of Alexandria, who grouped 1022 stars into 48 constellations during the 2nd century A.D. Although Ptolemy's Almagest does not include the co ...
Spectral Classification
... O and B stars are so powerful, they live for a very short time. They do not stray far from the area in which they were formed as they don't have the time. They therefore tend to cluster together in what we call OB1 associations. and contains all of the constellation of Orion. They constitute about 0 ...
... O and B stars are so powerful, they live for a very short time. They do not stray far from the area in which they were formed as they don't have the time. They therefore tend to cluster together in what we call OB1 associations. and contains all of the constellation of Orion. They constitute about 0 ...
hotstar_xrays
... The context of X-ray spectral observations of hot stars Hot stars are thought not to have outer convection zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do ha ...
... The context of X-ray spectral observations of hot stars Hot stars are thought not to have outer convection zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do ha ...
12-1 MAIN-SEQUENCE STARS
... system, and mass can flow from one star to the other through the inner Lagrangian point. Close binary stars evolve in complex ways because they can transfer mass from one star to the other. This explains why some binary systems contain a main-sequence star more massive than its giant companion—the A ...
... system, and mass can flow from one star to the other through the inner Lagrangian point. Close binary stars evolve in complex ways because they can transfer mass from one star to the other. This explains why some binary systems contain a main-sequence star more massive than its giant companion—the A ...
dm curvas de rotacion
... How does the star’s orbital velocity depend on the distribution of the galaxy mass? • Simplifying assumption: Spherical galaxy of mass Mtotal, radius R, and uniform density r Outside of galaxy: all galaxy mass Mtotal within the orbit radius r ...
... How does the star’s orbital velocity depend on the distribution of the galaxy mass? • Simplifying assumption: Spherical galaxy of mass Mtotal, radius R, and uniform density r Outside of galaxy: all galaxy mass Mtotal within the orbit radius r ...
TMSP Stellar Evolution & Life
... •The end result is that each element of matter has its own unique spectrum that can be seen as either a bright (emission) or dark (absorption) line, depending on how it is viewed. •And since this can be done (and has been done) in laboratories with elements heated to gaseous states, we now have a c ...
... •The end result is that each element of matter has its own unique spectrum that can be seen as either a bright (emission) or dark (absorption) line, depending on how it is viewed. •And since this can be done (and has been done) in laboratories with elements heated to gaseous states, we now have a c ...
ASTRONOMY AND ASTROPHYSICS Letter to the Editor Low
... be misleading since the theoretical calculations include only stellar photospheres while the stars still may be surrounded by dust envelopes and accretion disks. This would lead to excess emission in the NIR and make the stars appear younger than they actually are. Typical excess emission of classic ...
... be misleading since the theoretical calculations include only stellar photospheres while the stars still may be surrounded by dust envelopes and accretion disks. This would lead to excess emission in the NIR and make the stars appear younger than they actually are. Typical excess emission of classic ...
hubble_refurb
... The wispy, glowing, magenta structures in this image are the remains of a star 10 to 15 times the mass of the Sun that we would have seen exploding as a supernova 3,000 years ago. The remnant’s fast-moving gas is plowing into the surrounding gas of the galaxy, creating a supersonic shock wave in th ...
... The wispy, glowing, magenta structures in this image are the remains of a star 10 to 15 times the mass of the Sun that we would have seen exploding as a supernova 3,000 years ago. The remnant’s fast-moving gas is plowing into the surrounding gas of the galaxy, creating a supersonic shock wave in th ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... iii) It will experience mass loss (perhaps a substantial amount) by the shock and radiation pressure of the blast. f ) If the star in it final thermonuclear stages has too small a mass to supernova, it will lose its envelope through the creation of a planetary nebula (which will have little impact o ...
... iii) It will experience mass loss (perhaps a substantial amount) by the shock and radiation pressure of the blast. f ) If the star in it final thermonuclear stages has too small a mass to supernova, it will lose its envelope through the creation of a planetary nebula (which will have little impact o ...
Galaxies – Island universes
... • Many have later infalling matter which has been pulled on by nearby mass and thus doesn’t fall straight in. It settles into a rotating disk, arranging itself into a flat, roughly circularly orbiting plane of material • This material gradually condenses enough to initiate star formation. Then super ...
... • Many have later infalling matter which has been pulled on by nearby mass and thus doesn’t fall straight in. It settles into a rotating disk, arranging itself into a flat, roughly circularly orbiting plane of material • This material gradually condenses enough to initiate star formation. Then super ...
PHYSICS 1500 - ASTRONOMY TOTAL: 100 marks Section A Please
... (b) Halley is loosely packed ices with a small amount of rocky material. (c) Halley formed in the inner solar system and was ejected by Jupiter to the Kuiper belt. (d) Halley is really an S-type asteroid. (e) Halley was once a moon of Neptune and was ripped away by a large impact. ...
... (b) Halley is loosely packed ices with a small amount of rocky material. (c) Halley formed in the inner solar system and was ejected by Jupiter to the Kuiper belt. (d) Halley is really an S-type asteroid. (e) Halley was once a moon of Neptune and was ripped away by a large impact. ...
slides
... A star initially more massive than 8 solar masses will have a core heavier than the Chandrasekhar limit (1.4M☉ ) after the red giant stage. – electron degenerate pressure can not overcome the crushing force of gravity. It is too big to be a white dwarf! – Gravitational crush will overcome the electr ...
... A star initially more massive than 8 solar masses will have a core heavier than the Chandrasekhar limit (1.4M☉ ) after the red giant stage. – electron degenerate pressure can not overcome the crushing force of gravity. It is too big to be a white dwarf! – Gravitational crush will overcome the electr ...
Grossmugl Star Walk Installation
... 600 and 500 BC. This was the time when Babylon experienced one of its wealthiest periods under king Nebuchadnezzar II, democracy was invented in Athens and the city of Rome was still a small kingdom, far from the great empire it would later become. When stargazing at this historic site one can almos ...
... 600 and 500 BC. This was the time when Babylon experienced one of its wealthiest periods under king Nebuchadnezzar II, democracy was invented in Athens and the city of Rome was still a small kingdom, far from the great empire it would later become. When stargazing at this historic site one can almos ...
Homework #7 (Ch. 19)
... What do star clusters and associations have to do with star formation? 10. Chaisson Review and Discussion 19.18 Compare and contrast the observed properties of open star clusters and globular star clusters. 11. Chaisson Review and Discussion 19.19 How can we tell whether a star cluster is young or o ...
... What do star clusters and associations have to do with star formation? 10. Chaisson Review and Discussion 19.18 Compare and contrast the observed properties of open star clusters and globular star clusters. 11. Chaisson Review and Discussion 19.19 How can we tell whether a star cluster is young or o ...
Sun - UNT Physics
... WHAT ARE THE INVARIANTS IN THE UNIVERSE? “CONSTELLATIONS” CON: CONSTANT STELLAR: STAR ...
... WHAT ARE THE INVARIANTS IN THE UNIVERSE? “CONSTELLATIONS” CON: CONSTANT STELLAR: STAR ...
Fulltext PDF - Indian Academy of Sciences
... of eclipse. The spectral variations also have been recorded. The well established techniques help us to estimate the masses of the components as 1.1 M0 and about 0.6 M 0 . This, combined with other information, will give a clue on the nature of the smaller companion - it has to be a compact object. ...
... of eclipse. The spectral variations also have been recorded. The well established techniques help us to estimate the masses of the components as 1.1 M0 and about 0.6 M 0 . This, combined with other information, will give a clue on the nature of the smaller companion - it has to be a compact object. ...
Life in the Universe
... On a clear night, with 20/20 vision, one can see about 3,000 stars at a given time. Ancient astronomers traced out “pictures” using groups of these stars. “Group of Stars” in Latin constellations ...
... On a clear night, with 20/20 vision, one can see about 3,000 stars at a given time. Ancient astronomers traced out “pictures” using groups of these stars. “Group of Stars” in Latin constellations ...
Stars part 1
... hydrogen and helium. 1 or 2% of the star’s mass may contain iron, titanium, calcium, sodium ... ...
... hydrogen and helium. 1 or 2% of the star’s mass may contain iron, titanium, calcium, sodium ... ...
The Death of High Mass Stars
... searchlight is like a lighthouse, which we see as a pulsar if we happen to lie in the searchlight beam. ...
... searchlight is like a lighthouse, which we see as a pulsar if we happen to lie in the searchlight beam. ...
Laboratory Procedure (Word Format)
... In dealing with line of sight motions, astronomers call the velocities of approach negative (-) and velocities of recession positive (+). Let (VO) be the orbital velocity of the earth in km/sec, and (VS) be the radial velocity of the star relative to the sun. Then at time A, the motion of the star r ...
... In dealing with line of sight motions, astronomers call the velocities of approach negative (-) and velocities of recession positive (+). Let (VO) be the orbital velocity of the earth in km/sec, and (VS) be the radial velocity of the star relative to the sun. Then at time A, the motion of the star r ...
Astron 104 Laboratory #9 Cepheid Variable Stars
... • The apparent magnitude of the star, which is a measure of how much light we receive on Earth (i.e., how bright do we measure the star to be). • The absolute magnitude of the star, which is a measure of how much light it is actually radiating into space (i.e, how bright it actually is). • The star’ ...
... • The apparent magnitude of the star, which is a measure of how much light we receive on Earth (i.e., how bright do we measure the star to be). • The absolute magnitude of the star, which is a measure of how much light it is actually radiating into space (i.e, how bright it actually is). • The star’ ...
Lecture Eight (Powerpoint format) - Flash
... The collapse of the disk is arrested at the center once the gas begins to heat up and can support itself under its own weight. At this point, the central “core” is entirely molecular in composition, is a few hundreds of degrees at its surface, and has a radius of a few AU (comparable to the orbi ...
... The collapse of the disk is arrested at the center once the gas begins to heat up and can support itself under its own weight. At this point, the central “core” is entirely molecular in composition, is a few hundreds of degrees at its surface, and has a radius of a few AU (comparable to the orbi ...
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.