Stars, Galaxies, and the Universe Section 1 Distances to Stars
... • Stars vary in size and mass. • Stars such as the sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less mas ...
... • Stars vary in size and mass. • Stars such as the sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less mas ...
"Dark Matter in the Milky Way - how to find it using Gaia and other
... We have observations of cold gas that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths ...
... We have observations of cold gas that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths ...
astrophysics - The University of Sydney
... there’s a poster called The Southern Cross and the “Pointers” by Akira Fujii available from CSIRO Parkes Observatory. Ask students to order the stars by brightness, then show them the actual distances to the stars as shown in Figure 3. Alpha and Beta Centauri are almost the same brightness, but Beta ...
... there’s a poster called The Southern Cross and the “Pointers” by Akira Fujii available from CSIRO Parkes Observatory. Ask students to order the stars by brightness, then show them the actual distances to the stars as shown in Figure 3. Alpha and Beta Centauri are almost the same brightness, but Beta ...
Astronomy Assignment #1
... 13. How do the magnitudes of stars C and D in problem 4 compare? (Problem 4 synopsis: Stars C and D are the same distance from us, but star D is 10,000 times more luminous.) To answer this problem you need to use the rule regarding magnitudes and brightness’s: if two stars differ in magnitude by 5 m ...
... 13. How do the magnitudes of stars C and D in problem 4 compare? (Problem 4 synopsis: Stars C and D are the same distance from us, but star D is 10,000 times more luminous.) To answer this problem you need to use the rule regarding magnitudes and brightness’s: if two stars differ in magnitude by 5 m ...
Ursa Major, the Great Bear
... M101 is a splendid face-on galaxy, which shows a distinct asymmetry in long exposure photographs. The giant spiral disk of stars, dust, and gas is 170,000 light-years across, almost twice the size of our Milky Way Galaxy. M101 is estimated to contain at least one trillion stars. M101 lies on the e ...
... M101 is a splendid face-on galaxy, which shows a distinct asymmetry in long exposure photographs. The giant spiral disk of stars, dust, and gas is 170,000 light-years across, almost twice the size of our Milky Way Galaxy. M101 is estimated to contain at least one trillion stars. M101 lies on the e ...
D1 Stellar quantities (PPT)
... The only parameter that determines how much EM radiation the black body radiates for the given wavelength is its temperature. That is why the radiation emitted by an blackbody is often called thermal radiation. The hotter the blackbody, the more EM radiation at all wavelengths. • Black body emits en ...
... The only parameter that determines how much EM radiation the black body radiates for the given wavelength is its temperature. That is why the radiation emitted by an blackbody is often called thermal radiation. The hotter the blackbody, the more EM radiation at all wavelengths. • Black body emits en ...
Nature of Stars 2
... We can use Kepler’s 3rd Law* to determine the masses of the stars *Fortified with vitamin Newton! ...
... We can use Kepler’s 3rd Law* to determine the masses of the stars *Fortified with vitamin Newton! ...
Dark Matter in the Milky Way - how to find it using Gaia and other
... We have observations of cold gas that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths There are existing constraints on the Milky Way’s mass from other dynamical mode ...
... We have observations of cold gas that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths There are existing constraints on the Milky Way’s mass from other dynamical mode ...
Tour the sky`s reddest stars
... of stars by their spectral types, was so impressed with Y CVn that he called it “La Superba.” Scientists study a star’s spectrum by measuring the intensity of its light at different wavelengths. The standard spectral classes assign letters to stars based on their temperatures. From hottest to cooles ...
... of stars by their spectral types, was so impressed with Y CVn that he called it “La Superba.” Scientists study a star’s spectrum by measuring the intensity of its light at different wavelengths. The standard spectral classes assign letters to stars based on their temperatures. From hottest to cooles ...
HR4AGN Powerpoint Presentation-a
... • But how do we figure out how far away quasar is? • One way is to figure out its inherent luminosity and then compare it to its apparent luminosity because light follows the inverse square law: ...
... • But how do we figure out how far away quasar is? • One way is to figure out its inherent luminosity and then compare it to its apparent luminosity because light follows the inverse square law: ...
luminosity1
... • Now that we know the way things work on the H-R diagram, for stars that we can measure distance to using trigonometric parallax (triangulation) we can make use of these laws to calculate the distance to stars that are too far away to measure distance directly. • Here is what we know. • B = L/4πd2 ...
... • Now that we know the way things work on the H-R diagram, for stars that we can measure distance to using trigonometric parallax (triangulation) we can make use of these laws to calculate the distance to stars that are too far away to measure distance directly. • Here is what we know. • B = L/4πd2 ...
A little bit more to do. Stefan
... • Now that we know the way things work on the H-R diagram, for stars that we can measure distance to using trigonometric parallax (triangulation) we can make use of these laws to calculate the distance to stars that are too far away to measure distance directly. • Here is what we know. • B = L/4πd2 ...
... • Now that we know the way things work on the H-R diagram, for stars that we can measure distance to using trigonometric parallax (triangulation) we can make use of these laws to calculate the distance to stars that are too far away to measure distance directly. • Here is what we know. • B = L/4πd2 ...
Star Factories: Nuclear Fusion and the Creation of the Elements
... universe first formed, the only matter that existed was hydrogen, helium, and very tiny amounts of lithium. If this is true, then all other elements must have been created in stars. ...
... universe first formed, the only matter that existed was hydrogen, helium, and very tiny amounts of lithium. If this is true, then all other elements must have been created in stars. ...
2P24.pdf
... to study their properties with spatial resolution. This data, in combination with optical and near-infrared imaging will be used to separate the regions where there is active star formation from the zones where the older underlying population dominates the luminosity. Maps of the extinction and meta ...
... to study their properties with spatial resolution. This data, in combination with optical and near-infrared imaging will be used to separate the regions where there is active star formation from the zones where the older underlying population dominates the luminosity. Maps of the extinction and meta ...
Astronomy: Life Cycle of a Star
... _________________________________. Fusion happens when two lightweight atoms are forced together to form a heavier one, producing a lot of ________________. However, fusion can only occur at the incredibly high __________________ and ______________________________ found at the center of stars. Are S ...
... _________________________________. Fusion happens when two lightweight atoms are forced together to form a heavier one, producing a lot of ________________. However, fusion can only occur at the incredibly high __________________ and ______________________________ found at the center of stars. Are S ...
Properties of Ellipticals and Spirals
... Ellipticals: Velocities of stars in ellipticals are more or less random Velocity dispersions are responsible for the overall shape of galaxies. Oblate and Prolate Ellipticals – how that? Spiral: Velocities of stars in spirals are more ordered. Stars rotate around the galactic center in a disk surrou ...
... Ellipticals: Velocities of stars in ellipticals are more or less random Velocity dispersions are responsible for the overall shape of galaxies. Oblate and Prolate Ellipticals – how that? Spiral: Velocities of stars in spirals are more ordered. Stars rotate around the galactic center in a disk surrou ...
harrold_kajubi_astro1
... Very large uncertainty incurred through by-hand photometry (note B-V scales do not match) Spread resembles asymptotic (red) giant branches No evidence of main sequence Better photometry is needed to: Verify distance modulus from main sequence shift Verify cluster age from turn-off point ...
... Very large uncertainty incurred through by-hand photometry (note B-V scales do not match) Spread resembles asymptotic (red) giant branches No evidence of main sequence Better photometry is needed to: Verify distance modulus from main sequence shift Verify cluster age from turn-off point ...
Radio Telescopes Consolidation Activity
... Any value correctly calculated from the Hα wavelength in question 1 is acceptable. For example, λ = 6600 Angstroms gives z = 0.006 4. v = z x c. Using z = 0.003 gives 900 km s-1 Any answer consistent with value of z from question 3 is acceptable. For example, vrec = 1,800 km s-1 (for z = 0.006) 5. H ...
... Any value correctly calculated from the Hα wavelength in question 1 is acceptable. For example, λ = 6600 Angstroms gives z = 0.006 4. v = z x c. Using z = 0.003 gives 900 km s-1 Any answer consistent with value of z from question 3 is acceptable. For example, vrec = 1,800 km s-1 (for z = 0.006) 5. H ...
syn-any
... things as a whole – the relatively complete picture. • The is no (theoretical) limit to either the depth of analysis nor the most complete picture. • Very important in life and academics is the art of questioning (i.e. knowing when to ask for details and when to look for macro-picture) • The success ...
... things as a whole – the relatively complete picture. • The is no (theoretical) limit to either the depth of analysis nor the most complete picture. • Very important in life and academics is the art of questioning (i.e. knowing when to ask for details and when to look for macro-picture) • The success ...
Oldest SN
... the apparent brightness of these supernovae at their peak exists. We assume that these are canonical supernovae with an absolute magnitude of -19.6 and then derive their apparent magnitude from their distance. Both these objects would have been visible from the site. The age of these SNRs is determi ...
... the apparent brightness of these supernovae at their peak exists. We assume that these are canonical supernovae with an absolute magnitude of -19.6 and then derive their apparent magnitude from their distance. Both these objects would have been visible from the site. The age of these SNRs is determi ...
Target Stars for Earth-like Planet Searches with the Terrestrial
... (2) Using catalogued colors and magnitudes it is possible to calculate the basic parameters for an Earth-like planet near each of the stars, including the diameter of the Habitable Zone (HZ). For these purposes, the HZ is defined as the distance from the star at which an Earth-like planet would have ...
... (2) Using catalogued colors and magnitudes it is possible to calculate the basic parameters for an Earth-like planet near each of the stars, including the diameter of the Habitable Zone (HZ). For these purposes, the HZ is defined as the distance from the star at which an Earth-like planet would have ...
Separating Stars and Galaxies Based on Color
... define an object’s color as the (log) ratio of the fluxes in two filters. Due to the limited number of such filters, ambiguities between object types appear, as objects with very different spectra can have very similar colors. The Deep Lens Survey is a twenty square degree, ground-based, multi-band ...
... define an object’s color as the (log) ratio of the fluxes in two filters. Due to the limited number of such filters, ambiguities between object types appear, as objects with very different spectra can have very similar colors. The Deep Lens Survey is a twenty square degree, ground-based, multi-band ...
Spatial Structure Evolution of Star Clusters
... Stars concentrate progressively toward the center. The King model (1962) is understood as a combination of an isothermal sphere; i.e., dynamically relaxed in the inner part of the cluster, and tidal truncation by the Milky Way in the outer part. ...
... Stars concentrate progressively toward the center. The King model (1962) is understood as a combination of an isothermal sphere; i.e., dynamically relaxed in the inner part of the cluster, and tidal truncation by the Milky Way in the outer part. ...
Galaxy Classification - VCI
... galaxies: SBa, SBb, SBc. Our own Milky Way is probably an SBb type galaxy, similar to Andromeda, but with a central bar. ...
... galaxies: SBa, SBb, SBc. Our own Milky Way is probably an SBb type galaxy, similar to Andromeda, but with a central bar. ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.