Lecture 13 - Star Formation
... A star has 4 times the mass and 128 times the luminosity of the Sun. The star's lifetime will be ____ times that of Sun. A) 32 B) 4 C) 1 D) ¼ E) 1/32 ...
... A star has 4 times the mass and 128 times the luminosity of the Sun. The star's lifetime will be ____ times that of Sun. A) 32 B) 4 C) 1 D) ¼ E) 1/32 ...
Astronomical Distance Ladder
... d cluster d t sin This proper motion technique is capable of giving reliable distances up to around 800 parsecs. With the distances to many stars in the galaxy calculated by parallax different ways to calculate distance was needed to extend the astronomical distance ladder. It was also discovere ...
... d cluster d t sin This proper motion technique is capable of giving reliable distances up to around 800 parsecs. With the distances to many stars in the galaxy calculated by parallax different ways to calculate distance was needed to extend the astronomical distance ladder. It was also discovere ...
30galaxies and the universe
... that pulsate in brightness because of the expansion c. RR Lyrae variables and contraction of their layers ______ 2. Stars that have periods of pulsations between 1.5 d. Sagittarius e. variable stars hours and 1.2 days, and on average, have the same luminosity ...
... that pulsate in brightness because of the expansion c. RR Lyrae variables and contraction of their layers ______ 2. Stars that have periods of pulsations between 1.5 d. Sagittarius e. variable stars hours and 1.2 days, and on average, have the same luminosity ...
jackie822 beanerbutt777 life cycle of a star
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
Issue 118 - Apr 2014
... our guest speaker. A former president of the American Association of Variable Star Observers, Dr. Motto will talk about variable stars.] Variable stars are stars that change brightness. Some important types of variable stars to observe are: Cepheids - Named after Delta Cephei, these luminous stars b ...
... our guest speaker. A former president of the American Association of Variable Star Observers, Dr. Motto will talk about variable stars.] Variable stars are stars that change brightness. Some important types of variable stars to observe are: Cepheids - Named after Delta Cephei, these luminous stars b ...
Black Hole
... The Sun would have to shine for ~ 800 billion years at its present luminosity to give off 1046 joules. At the moment of collapse, the power output of a Type II supernova is comparable to that of all the stars in the observed Universe combined. ...
... The Sun would have to shine for ~ 800 billion years at its present luminosity to give off 1046 joules. At the moment of collapse, the power output of a Type II supernova is comparable to that of all the stars in the observed Universe combined. ...
Microsoft Word 97
... gamma-rays and those bursts of gamma rays that last only minutes. b) The gamma ray bursts, which were seen at random places in the sky, happened roughly once per day. c) Though some models suggested that they are produced within our galaxy – either very close to us, or in very extended halo – more r ...
... gamma-rays and those bursts of gamma rays that last only minutes. b) The gamma ray bursts, which were seen at random places in the sky, happened roughly once per day. c) Though some models suggested that they are produced within our galaxy – either very close to us, or in very extended halo – more r ...
Camelopardalis-Better-Know-A-Constellation
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
An analogy
... • MHI/Mtot increases from E to S --> fuel for star formation also increases --> SFR should increase from E to S ...
... • MHI/Mtot increases from E to S --> fuel for star formation also increases --> SFR should increase from E to S ...
Apparent Magnitude - RanelaghALevelPhysics
... emitted per second (units of Watts). • The Sun’s luminosity is about 4 x 1026 W. • The most luminous stars have a luminosity of about million times that of the Sun! ...
... emitted per second (units of Watts). • The Sun’s luminosity is about 4 x 1026 W. • The most luminous stars have a luminosity of about million times that of the Sun! ...
The Celestial Sphere - Department of Physics and Astronomy
... However some stars show small motions, these are due again to the motion of the Earth. An object that moves 1 second of arc in the sky (1/3600 of a degree) as the Earth moves 1 AU in its orbit in 1 ...
... However some stars show small motions, these are due again to the motion of the Earth. An object that moves 1 second of arc in the sky (1/3600 of a degree) as the Earth moves 1 AU in its orbit in 1 ...
TF_final3 - Arecibo Observatory
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
The Formation of Stars and Solar Systems
... new stars. Although the star formation process is not fully understood, there is observational evidence that most stars are born in the densest parts of molecular clouds. NASA, 2005 ...
... new stars. Although the star formation process is not fully understood, there is observational evidence that most stars are born in the densest parts of molecular clouds. NASA, 2005 ...
DTU9ePPTChap13 - Faculty Lounge : Astronomy
... eventually produces an iron core. A high-mass star dies in a supernova explosion that ejects most of the star’s matter into space at very high speeds. This Type II supernova is triggered by the gravitational collapse and subsequent bounce of the doomed star’s core. Neutrinos were detected from Super ...
... eventually produces an iron core. A high-mass star dies in a supernova explosion that ejects most of the star’s matter into space at very high speeds. This Type II supernova is triggered by the gravitational collapse and subsequent bounce of the doomed star’s core. Neutrinos were detected from Super ...
public_lector_10
... The dark halo was built up from mergers of smaller sub-halos Saw spiral structure developing in the gas Merging of galaxies is still going on now ...
... The dark halo was built up from mergers of smaller sub-halos Saw spiral structure developing in the gas Merging of galaxies is still going on now ...
Conference Summary Richard Ellis (Caltech) ITALIA
... • Masses and colors of z~2-3 red galaxies (Henriques, Conselice) • Evidence of star formation thresholds (Faber) • Timescale of truncation and AGN feedback (Somerville, Faber) • Morphology versus color (red disks) ...
... • Masses and colors of z~2-3 red galaxies (Henriques, Conselice) • Evidence of star formation thresholds (Faber) • Timescale of truncation and AGN feedback (Somerville, Faber) • Morphology versus color (red disks) ...
Unit 1
... • Photons have a difficult time moving through a star’s atmosphere • If the photon has the right energy, it will be absorbed by an atom and raise an electron to a higher energy level • Creates absorption spectra, a unique “fingerprint” for the star’s composition. The strength of this spectra is dete ...
... • Photons have a difficult time moving through a star’s atmosphere • If the photon has the right energy, it will be absorbed by an atom and raise an electron to a higher energy level • Creates absorption spectra, a unique “fingerprint” for the star’s composition. The strength of this spectra is dete ...
STAR FORMATION
... • If the protostar's mass is less than about 8% of the Sun's mass it is insufficient to compress the center to temperatures and densities adequate to allow ordinary fusion -- THE LOWER MASS LIMIT • Such failed stars are called brown dwarfs. • Most astronomers make a further distinction between brown ...
... • If the protostar's mass is less than about 8% of the Sun's mass it is insufficient to compress the center to temperatures and densities adequate to allow ordinary fusion -- THE LOWER MASS LIMIT • Such failed stars are called brown dwarfs. • Most astronomers make a further distinction between brown ...
US - Real Science
... Around one quarter of all large stars are born in starburst galaxies such as this. They spawn stars up to a thousand times faster than the Milky Way. In most starbursts the surge in starbirth is triggered when two galaxies come too close together. Mutual attraction between the galaxies causes immens ...
... Around one quarter of all large stars are born in starburst galaxies such as this. They spawn stars up to a thousand times faster than the Milky Way. In most starbursts the surge in starbirth is triggered when two galaxies come too close together. Mutual attraction between the galaxies causes immens ...
The HR Diagram - Faculty Web Pages
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
... brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an im ...
Syllabus - University of Texas Rio Grande Valley
... …). State the types of electromagnetic spectra (radio, visible light, …) in order from lower energy to higher energy. If one photon is of a higher energy than another, state which one has a longer wavelength. If one photon is of a higher energy than another, state which one has a higher frequency. D ...
... …). State the types of electromagnetic spectra (radio, visible light, …) in order from lower energy to higher energy. If one photon is of a higher energy than another, state which one has a longer wavelength. If one photon is of a higher energy than another, state which one has a higher frequency. D ...
Click here to the PowerPoint
... Make sure you understand each step, take down key notes (purple boxes) and ask questions if you don’t get it. You must be able to describe processes in your own words, and remember each stage in order! ...
... Make sure you understand each step, take down key notes (purple boxes) and ask questions if you don’t get it. You must be able to describe processes in your own words, and remember each stage in order! ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... Since distance α 1 / parallax, Spica must be at twice the distance of Canopus. (The numbers are 100 pc and 200 pc, but you don’t need to know that.) The more distant star (Spica) appears fainter. Since it is twice as distant as Canopus, it appears 4 times fainter, or ¼ as bright. We could use the ma ...
... Since distance α 1 / parallax, Spica must be at twice the distance of Canopus. (The numbers are 100 pc and 200 pc, but you don’t need to know that.) The more distant star (Spica) appears fainter. Since it is twice as distant as Canopus, it appears 4 times fainter, or ¼ as bright. We could use the ma ...
Activity 4
... In this equation, m is the apparent magnitude and M is the absolute magnitude. Apparent magnitude can be easily measured from a CCD image, but absolute magnitude takes some work. Cepheid variables ...
... In this equation, m is the apparent magnitude and M is the absolute magnitude. Apparent magnitude can be easily measured from a CCD image, but absolute magnitude takes some work. Cepheid variables ...
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.