ppt
... lists this as an A5 V star, but it is a g Dor variable which have spectral types F0-F2. Tautenburg spectra confirm that it is F-type 1SIMBAD ...
... lists this as an A5 V star, but it is a g Dor variable which have spectral types F0-F2. Tautenburg spectra confirm that it is F-type 1SIMBAD ...
Discovery of White Dwarfs—8 Oct
... Main-sequence or dwarf stars Giants Horizontal-branch stars White dwarfs are too faint for these observations. A star lives a long time as a dwarf. It is on the main sequence. When it runs out of fuel, it becomes a giant and subsequently “traces out the giant branch.” ...
... Main-sequence or dwarf stars Giants Horizontal-branch stars White dwarfs are too faint for these observations. A star lives a long time as a dwarf. It is on the main sequence. When it runs out of fuel, it becomes a giant and subsequently “traces out the giant branch.” ...
HR Diagram
... Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating – alternately growing bigger and smaller – ...
... Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating – alternately growing bigger and smaller – ...
Deriving the Isoradius Lines (optional, mathematical
... An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around the diagram. The options panel allows you to control the variables plotted on the x-axis: (temperature, BV, or spectral type) and those plotted on the y- ...
... An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around the diagram. The options panel allows you to control the variables plotted on the x-axis: (temperature, BV, or spectral type) and those plotted on the y- ...
Chap1-Introduction - Groupe d`astrophysique de UdeM
... Overview of observational techniques Transit Photometric method consisting of measuring the host star flux variation due to the planet primary and secondary eclipses. Most prolific method (largely from the Kepler mission). Works only for systems with an inclination close to 90°. Transit probab ...
... Overview of observational techniques Transit Photometric method consisting of measuring the host star flux variation due to the planet primary and secondary eclipses. Most prolific method (largely from the Kepler mission). Works only for systems with an inclination close to 90°. Transit probab ...
TAP702-0: Red shift - Teaching Advanced Physics
... When the stars are at C and the point diametrically opposite to C respectively, then both will have their 589.0 nm spectral line red shifted by 0.13 nm, as both will have the same velocity relative to the Earth (question 4). When they move towards A and B, however, their velocities relative to Earth ...
... When the stars are at C and the point diametrically opposite to C respectively, then both will have their 589.0 nm spectral line red shifted by 0.13 nm, as both will have the same velocity relative to the Earth (question 4). When they move towards A and B, however, their velocities relative to Earth ...
TAP702-0: Red shift - Teaching Advanced Physics
... When the stars are at C and the point diametrically opposite to C respectively, then both will have their 589.0 nm spectral line red shifted by 0.13 nm, as both will have the same velocity relative to the Earth (question 4). When they move towards A and B, however, their velocities relative to Earth ...
... When the stars are at C and the point diametrically opposite to C respectively, then both will have their 589.0 nm spectral line red shifted by 0.13 nm, as both will have the same velocity relative to the Earth (question 4). When they move towards A and B, however, their velocities relative to Earth ...
Science Grade 08 Unit 11 Exemplar Lesson 02: Classifying Stars
... This unit bundles student expectations that address components and characteristics of the universe. Students learn that stars and galaxies are part of the universe and how they can be classified by their characteristics. Prior to this unit, in Grade 8, students studied the effects resulting from cyc ...
... This unit bundles student expectations that address components and characteristics of the universe. Students learn that stars and galaxies are part of the universe and how they can be classified by their characteristics. Prior to this unit, in Grade 8, students studied the effects resulting from cyc ...
Document
... Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted gas. Thus the iron abundances are artifically low, but the Carbon, ...
... Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted gas. Thus the iron abundances are artifically low, but the Carbon, ...
PHYS3380_111115_bw - The University of Texas at Dallas
... In the 1930’s supernovae were recognised as a separate class of objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supern ...
... In the 1930’s supernovae were recognised as a separate class of objects to novae (meaning new stars). • So-called by Fritz Zwicky, after Edwin Hubble estimated distance to Andromeda galaxy (through Cepheids) • Hence the luminosity of the “nova” discovered in 1885 in Andromeda was determined • Supern ...
The Naked Eye Stars as Data Supporting Galileo`s
... If stars are not suns scattered through space then there is no reason for the real sky to look like the top row. For example, if the stars are simply bodies distributed along a spherical shell centered on Earth as in geocentric theories then there is no reason why their numbers by brightness might n ...
... If stars are not suns scattered through space then there is no reason for the real sky to look like the top row. For example, if the stars are simply bodies distributed along a spherical shell centered on Earth as in geocentric theories then there is no reason why their numbers by brightness might n ...
Spatial distribution of stars in the Milky Way
... Andromeda galaxy he found that the disk stars in M31 were like nearby disk stars in our Galaxy, while the bulge stars resembled those of the Galaxy's globular clusters. ...
... Andromeda galaxy he found that the disk stars in M31 were like nearby disk stars in our Galaxy, while the bulge stars resembled those of the Galaxy's globular clusters. ...
Astronomical Formulae
... Where D is the diameter of the objective in inches Atmospheric conditions seldom permit Theta > 0.5". The Dawes Limit is one half the angular diameter of the Airy (diffraction) disc, so that the edge of one disc does not extend beyond the center of the other). The working value is two times the Dawe ...
... Where D is the diameter of the objective in inches Atmospheric conditions seldom permit Theta > 0.5". The Dawes Limit is one half the angular diameter of the Airy (diffraction) disc, so that the edge of one disc does not extend beyond the center of the other). The working value is two times the Dawe ...
Westerlund 1 : A Super-Star Cluster within the Milky Way
... In the Milky Way massive clusters are rare. The most massive examples known have M and include NGC 3603, plus the Arches and Quintuplet clusters in the Galactic Centre. Westerlund 1 (Wd1) is a highly reddened (E(B-V)=4.5) open Galactic cluster (G339.55, ...
... In the Milky Way massive clusters are rare. The most massive examples known have M and include NGC 3603, plus the Arches and Quintuplet clusters in the Galactic Centre. Westerlund 1 (Wd1) is a highly reddened (E(B-V)=4.5) open Galactic cluster (G339.55, ...
Binocular Objects (MS Word)
... Sagittarius contains more Messier objects than any other constellation. The best way to identify them is to take them one by one. The beginner will have to be careful not to confuse the various objects. The principal stars of Sagittarius form the famous “Teapot” asterism. The brightest part of the M ...
... Sagittarius contains more Messier objects than any other constellation. The best way to identify them is to take them one by one. The beginner will have to be careful not to confuse the various objects. The principal stars of Sagittarius form the famous “Teapot” asterism. The brightest part of the M ...
The Milky Way Galaxy
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
Universe 8e Lecture Chapter 24 Galaxies
... Rich, regular clusters contain mostly elliptical and lenticular galaxies; irregular clusters contain spiral, barred spiral, and irregular galaxies along with ellipticals. Giant elliptical galaxies are often found near the centers of rich clusters. ...
... Rich, regular clusters contain mostly elliptical and lenticular galaxies; irregular clusters contain spiral, barred spiral, and irregular galaxies along with ellipticals. Giant elliptical galaxies are often found near the centers of rich clusters. ...
Physics 1040 Constellation paper
... both Callisto and Arcas into the sky as bears, to prevent the killing, these became known to us as Ursa Major and Ursa Minor or the Great Bear and the Little Bear. It is said that Zeus threw both Callisto and Arcas into the sky by their tails which is why both bears in the sky have very long tails. ...
... both Callisto and Arcas into the sky as bears, to prevent the killing, these became known to us as Ursa Major and Ursa Minor or the Great Bear and the Little Bear. It is said that Zeus threw both Callisto and Arcas into the sky by their tails which is why both bears in the sky have very long tails. ...
- University of Manitoba
... the associated bright region to the left of the nucleus, one can more clearly see the distinction between the two peak brightness values, and perhaps the presence of dust and gas covering one single bright region. ...
... the associated bright region to the left of the nucleus, one can more clearly see the distinction between the two peak brightness values, and perhaps the presence of dust and gas covering one single bright region. ...
Recent science results from VLTI commissioning
... • What is it? Single? Binary? Cluster? What is its current mass loss rate exactly? What is its or their mass? • What will it become? Normal star after more eruptions? Collapse into SN or hypernova? • Is it rotating? What is the origin of the 5.5yr periodicity in some lines and x-rays? Is there a mas ...
... • What is it? Single? Binary? Cluster? What is its current mass loss rate exactly? What is its or their mass? • What will it become? Normal star after more eruptions? Collapse into SN or hypernova? • Is it rotating? What is the origin of the 5.5yr periodicity in some lines and x-rays? Is there a mas ...
second grade - Math/Science Nucleus
... people would look into the night sky and wonder what was in "outer space." They developed stories on the groups of stars. Astronomers use 88 constellations to divide up the heavens. 2. Give each student one of the constellations and have them imagine what the constellation may look like in the sky. ...
... people would look into the night sky and wonder what was in "outer space." They developed stories on the groups of stars. Astronomers use 88 constellations to divide up the heavens. 2. Give each student one of the constellations and have them imagine what the constellation may look like in the sky. ...
ppt
... – Large increase in numbers of both early- and late-type X-ray stars in LMC – 50% increase in number of candidate X-ray binaries ...
... – Large increase in numbers of both early- and late-type X-ray stars in LMC – 50% increase in number of candidate X-ray binaries ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.