distant stars nearby star parallax angle The principle of geometrical
... didn’t know the distances to these stars, we wouldn’t know that Betelgeuse is a red giant star, with a much greater intrinsic brightness than Vega (and much larger diameter). Nor would we know that many stars visible in the night sky are much like the Sun, but just much, much farther away so they ap ...
... didn’t know the distances to these stars, we wouldn’t know that Betelgeuse is a red giant star, with a much greater intrinsic brightness than Vega (and much larger diameter). Nor would we know that many stars visible in the night sky are much like the Sun, but just much, much farther away so they ap ...
I Cloudy with a Chance of Making a star is no easy thing
... gas. Some grow much bigger than others, and the losers may be ejected from the cluster altogether, creating a class of stellar runts that roam the galaxy. This picture, called competitive accretion, has been championed by Ian Bonnell of the University of St. Andrews, Matthew Bate of the University o ...
... gas. Some grow much bigger than others, and the losers may be ejected from the cluster altogether, creating a class of stellar runts that roam the galaxy. This picture, called competitive accretion, has been championed by Ian Bonnell of the University of St. Andrews, Matthew Bate of the University o ...
Lecture 19 Brightness Units
... • For historical reasons, luminosity is plotted up and temperature towards left. • Each star is one point on the diagram ...
... • For historical reasons, luminosity is plotted up and temperature towards left. • Each star is one point on the diagram ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Important - think about what we are looking at when we observe a cluster. We are seeing a “freeze-frame” picture at a particular age. We see how stars of different masse ...
... different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Important - think about what we are looking at when we observe a cluster. We are seeing a “freeze-frame” picture at a particular age. We see how stars of different masse ...
ppt
... • An open cluster is a group of up to a few thousand stars that were formed from the same giant molecular cloud, and are still gravitationally bound to each other • Open clusters are found only in spiral and irregular galaxies, in which active star formation is occurring. • The Pleiades is an open c ...
... • An open cluster is a group of up to a few thousand stars that were formed from the same giant molecular cloud, and are still gravitationally bound to each other • Open clusters are found only in spiral and irregular galaxies, in which active star formation is occurring. • The Pleiades is an open c ...
Astronomy_Stellar_Evolution_and_Type_II_Supernovae_Exam
... 5) This object was the first of its kind to have its diameter measured with “Michelson's Beam Interferometer” ...
... 5) This object was the first of its kind to have its diameter measured with “Michelson's Beam Interferometer” ...
death_low_mass
... forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies s ...
... forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies s ...
Astronomy Worksheet
... 5. Often absorption lines will present as broad, V-shaped notches, in some cases 50 A or more. These are often caused by molecular absorption instead of absorption from a single element, and are known as molecular bands. In addition to gases around stars absorbing energy, Earth’s own atmosphere abso ...
... 5. Often absorption lines will present as broad, V-shaped notches, in some cases 50 A or more. These are often caused by molecular absorption instead of absorption from a single element, and are known as molecular bands. In addition to gases around stars absorbing energy, Earth’s own atmosphere abso ...
NGC 3370 Spiral Galaxy
... forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies s ...
... forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies s ...
Star Life Cycle Web Activity
... section only. Read this entire page. You may go to the other sections if you have time. An H-R diagram shows a wide array of stars plotted on a graph showing absolute magnitude (or luminosity) versus surface temperature (not core temperature). Notice most of the stars are in the main sequence, yet s ...
... section only. Read this entire page. You may go to the other sections if you have time. An H-R diagram shows a wide array of stars plotted on a graph showing absolute magnitude (or luminosity) versus surface temperature (not core temperature). Notice most of the stars are in the main sequence, yet s ...
Joining the Party - Lincoln-Sudbury Regional High School
... solar masses embedded in small dark molecular clouds. These stars have not yet quite reached the main sequence, but they are getting there. At least, we suspect so: these small stars evolve so slowly that we won’t be around long enough to actually see them arrive! ...
... solar masses embedded in small dark molecular clouds. These stars have not yet quite reached the main sequence, but they are getting there. At least, we suspect so: these small stars evolve so slowly that we won’t be around long enough to actually see them arrive! ...
Major Stars of the Orion Constellation
... by changes in the actual size of the star's atmosphere. According to Robert Burnham, Jr. (1931-93), Betelgeuse is the only marked variable among the first magnitude stars as well as the 11th brightest star in the sky. It is a well known semi-regular, pulsating variable, whose main period appears to ...
... by changes in the actual size of the star's atmosphere. According to Robert Burnham, Jr. (1931-93), Betelgeuse is the only marked variable among the first magnitude stars as well as the 11th brightest star in the sky. It is a well known semi-regular, pulsating variable, whose main period appears to ...
Astronomy Chapter 17 – Galaxies A. Main Ideas 1. Discovering
... ⇒ All galaxies are extremely distant from Earth, the nearest is more than 150,000 light-year away. Few can be seen with the naked eye. In the Northern Hemisphere the galaxy M31 appears as a pale smudge in the constellation Andromeda. ⇒ In the 18th and 19 centuries astronomers began catalogue the obj ...
... ⇒ All galaxies are extremely distant from Earth, the nearest is more than 150,000 light-year away. Few can be seen with the naked eye. In the Northern Hemisphere the galaxy M31 appears as a pale smudge in the constellation Andromeda. ⇒ In the 18th and 19 centuries astronomers began catalogue the obj ...
slides
... Interstellar gas and dust clouds (called nebulae) which could evolve into stars are abundant in galaxies, concentrated in the galactic disk. – They could span few to hundreds of light years in size and have masses many thousand times the Sun. – They are very cold (10-20K) low-density clouds, 102—106 ...
... Interstellar gas and dust clouds (called nebulae) which could evolve into stars are abundant in galaxies, concentrated in the galactic disk. – They could span few to hundreds of light years in size and have masses many thousand times the Sun. – They are very cold (10-20K) low-density clouds, 102—106 ...
Be Stars
... In all main sequence stars the outward thermal pressure from the hot core is balanced by the inward gravitational pressure from the star´s overlying layers. ...
... In all main sequence stars the outward thermal pressure from the hot core is balanced by the inward gravitational pressure from the star´s overlying layers. ...
Formation of Globular Clusters: In and Out of Dwarf Galaxies
... • Globular clusters may form in giant molecular clouds in progenitor galaxies at intermediate redshifts • Model explains observed sizes, masses, ages, metallicities • Dynamical evolution explains the present mass function and may be important for metallicity bimodality • Red clusters in the Galaxy a ...
... • Globular clusters may form in giant molecular clouds in progenitor galaxies at intermediate redshifts • Model explains observed sizes, masses, ages, metallicities • Dynamical evolution explains the present mass function and may be important for metallicity bimodality • Red clusters in the Galaxy a ...
Chapter 11 Surveying the Stars How do we measure stellar
... We can determine a star’s luminosity if we can measure its distance and apparent brightness: Luminosity = 4π (distance)2 × (Brightness) ...
... We can determine a star’s luminosity if we can measure its distance and apparent brightness: Luminosity = 4π (distance)2 × (Brightness) ...
center of mass
... 20. In a given volume of space the Red Dwarf (or lower main sequence) stars are the most abundant, however, on many H-R diagrams very few of these stars are plotted. Why? a. Photographic film and CCDs both have low sensitivity to lowenergy red photons. b. They are so very distant that parallax angle ...
... 20. In a given volume of space the Red Dwarf (or lower main sequence) stars are the most abundant, however, on many H-R diagrams very few of these stars are plotted. Why? a. Photographic film and CCDs both have low sensitivity to lowenergy red photons. b. They are so very distant that parallax angle ...
Chapter 09
... 20. In a given volume of space the Red Dwarf (or lower main sequence) stars are the most abundant, however, on many H-R diagrams very few of these stars are plotted. Why? a. Photographic film and CCDs both have low sensitivity to lowenergy red photons. b. They are so very distant that parallax angle ...
... 20. In a given volume of space the Red Dwarf (or lower main sequence) stars are the most abundant, however, on many H-R diagrams very few of these stars are plotted. Why? a. Photographic film and CCDs both have low sensitivity to lowenergy red photons. b. They are so very distant that parallax angle ...
Active Galaxies
... •Galaxies that emit most of their light in IR - LIR > 1012 Lsun •Few in local universe; most beyond z > 1 •Nearly all are undergoing mergers - forming E’s •IR light is likely a combination of dust reprocessed AGN emission and starbursts. •Some AGN may manifest as ULIRGs during different stages of ...
... •Galaxies that emit most of their light in IR - LIR > 1012 Lsun •Few in local universe; most beyond z > 1 •Nearly all are undergoing mergers - forming E’s •IR light is likely a combination of dust reprocessed AGN emission and starbursts. •Some AGN may manifest as ULIRGs during different stages of ...
Siriusposter
... white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal companions, just like the Sirius system. At optical wavelengths the white dwarfs are unresolv ...
... white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal companions, just like the Sirius system. At optical wavelengths the white dwarfs are unresolv ...
Here
... •Flat-fielding: pixels do not respond uniformly. Need to measure the individual response of the pixels by “observing” a diffuse screen or black twilight sky. •Calibration: Need to observe some standard stars, of known brightness to determine how many counts correspond to a given flux or magnitude. • ...
... •Flat-fielding: pixels do not respond uniformly. Need to measure the individual response of the pixels by “observing” a diffuse screen or black twilight sky. •Calibration: Need to observe some standard stars, of known brightness to determine how many counts correspond to a given flux or magnitude. • ...
• This chapter concentrates on five goals:
... The second goal for the chapter is to find out how much energy the stars emit. • Absolute visual magnitude refers to visible light. • However, you want to know the total output—including all types of radiation. – Hot stars emit a great deal of ultraviolet radiation that you can’t see. – Cool stars e ...
... The second goal for the chapter is to find out how much energy the stars emit. • Absolute visual magnitude refers to visible light. • However, you want to know the total output—including all types of radiation. – Hot stars emit a great deal of ultraviolet radiation that you can’t see. – Cool stars e ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.