Watching Galaxies Form Near the Beginning of Time
... Evidence for global winds escaping systems Exist in groupings with bright galaxies/AGN Are these the early units predicted by hierarchical schemes (and fitting dark-matter ...
... Evidence for global winds escaping systems Exist in groupings with bright galaxies/AGN Are these the early units predicted by hierarchical schemes (and fitting dark-matter ...
- Amazing Space, STScI
... Eta Carinae is an extremely massive, unstable star in the final stages of its life. It is approaching the point at which it will die in a titanic explosion called a supernova. About 150 years ago, Eta Carinae experienced a huge outburst that sent gas billowing away from the star. These lobes of gas ...
... Eta Carinae is an extremely massive, unstable star in the final stages of its life. It is approaching the point at which it will die in a titanic explosion called a supernova. About 150 years ago, Eta Carinae experienced a huge outburst that sent gas billowing away from the star. These lobes of gas ...
SOLUTIONS ASTROPHYSICS – OPTION D 2015-17
... The diagram below shows the grid of an HR diagram, on which the positions of selected stars are shown. (LS = luminosity of the Sun.) ...
... The diagram below shows the grid of an HR diagram, on which the positions of selected stars are shown. (LS = luminosity of the Sun.) ...
Extension worksheet – Topic 6 - Cambridge Resources for the IB
... brightness is made difficult by the presence of dust in the interstellar medium. Suggest the effect this has on the measured distance to the star. ...
... brightness is made difficult by the presence of dust in the interstellar medium. Suggest the effect this has on the measured distance to the star. ...
White Dwarfs
... D: Metals spontaneously decay to lighter elements during the 10 billion year age of the globular cluster. ...
... D: Metals spontaneously decay to lighter elements during the 10 billion year age of the globular cluster. ...
Chapter 28 Stars and Their Characteristics
... Apparent Magnitude- Apparent Magnitude is a how bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as ...
... Apparent Magnitude- Apparent Magnitude is a how bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as ...
Astronomy 114 Problem Set # 7 Due: 30 Apr 2007 SOLUTIONS 1
... gravitational pull at some radius R is induced by the mass within R, we denote it M(R). For the centrifugal force, we have ...
... gravitational pull at some radius R is induced by the mass within R, we denote it M(R). For the centrifugal force, we have ...
PhD Qualifying Exam (2010) --
... (a) If the equation of state of gas for a star is P K , prove that the condition for dynamic stability is 4 3 . (4 points) (b) The equation of state for non-relativistic degeneracy gas can be written as P K 5 3 . Estimate the mass-radius relation of this degenerate star. (3 points) (c) ...
... (a) If the equation of state of gas for a star is P K , prove that the condition for dynamic stability is 4 3 . (4 points) (b) The equation of state for non-relativistic degeneracy gas can be written as P K 5 3 . Estimate the mass-radius relation of this degenerate star. (3 points) (c) ...
Introduction:
... Intended Audience: Discovery (World Service); Leading Edge, Frontiers (Radio 4) ...
... Intended Audience: Discovery (World Service); Leading Edge, Frontiers (Radio 4) ...
Main-sequence stage Stellar lifetimes
... – Low-mass stars: the RR Lyrae variables are white horizontalbranch stars – Type II Cepheids are also low-mass stars. ...
... – Low-mass stars: the RR Lyrae variables are white horizontalbranch stars – Type II Cepheids are also low-mass stars. ...
Bubble Nebulae Around Ultra-luminous X
... remnants of Population III stars to the formation of supermassive black holes. Only a handful of radio detections of ULXs have been made so far. These sources all show large nebulae (>50 pc) that are likely powered by continuous energy input from the ULX, in the same manner as the W50 nebula is powe ...
... remnants of Population III stars to the formation of supermassive black holes. Only a handful of radio detections of ULXs have been made so far. These sources all show large nebulae (>50 pc) that are likely powered by continuous energy input from the ULX, in the same manner as the W50 nebula is powe ...
What We Know About Stars So Far
... graph using this system (comparing surface temperature and luminosity), you will find that the stars fall into groups. ...
... graph using this system (comparing surface temperature and luminosity), you will find that the stars fall into groups. ...
Handout Life of Stars
... A star begins its life as a cloud of dust and gas (mainly hydrogen) known as a nebula. A protostar is formed when gravity causes the dust and gas of a nebula to clump together in a process called accretion. As gravity continues to pull ever more matter inward towards the core, its temperature, press ...
... A star begins its life as a cloud of dust and gas (mainly hydrogen) known as a nebula. A protostar is formed when gravity causes the dust and gas of a nebula to clump together in a process called accretion. As gravity continues to pull ever more matter inward towards the core, its temperature, press ...
ref star birth - russballard.com
... set the scene for the next generation of stars. First, the new stars produce strong stellar winds which eat away and compress the edges of the cloud. Some of the stars even supernova. Parts of the cloud then become so dense that a cluster of new massive stars forms, along with a new stellar wind. Th ...
... set the scene for the next generation of stars. First, the new stars produce strong stellar winds which eat away and compress the edges of the cloud. Some of the stars even supernova. Parts of the cloud then become so dense that a cluster of new massive stars forms, along with a new stellar wind. Th ...
Calculating Main Sequence Lifetimes
... If we remember that the Sun’s mass is 2 × 10 Kg, and knowing the stellar mass, we can calculate the period in which the star burns Hydrogen, which the time it stays as a main sequence star. The star turns off: the star exhausts the Hydrogen in its core and it continues to burn it in shells.. For a ‘ ...
... If we remember that the Sun’s mass is 2 × 10 Kg, and knowing the stellar mass, we can calculate the period in which the star burns Hydrogen, which the time it stays as a main sequence star. The star turns off: the star exhausts the Hydrogen in its core and it continues to burn it in shells.. For a ‘ ...
Lecture 6: Main Sequence Stars
... heavy elements are ionised and create free electrons. These electrons can bind with H to make H-‐ ions which have a very high opacity (you destroy them with a photon and then they recombine) ...
... heavy elements are ionised and create free electrons. These electrons can bind with H to make H-‐ ions which have a very high opacity (you destroy them with a photon and then they recombine) ...
Definitions
... Blackbody – is a hypothetical body that is a perfect absorber and emitter of EMR C spectrum – consists of a continuous range of frequencies w/o either bright or dark lines, appearing as a continuous range of colours E spectrum – consists of only radiation at a number of discrete wavelengths, appeari ...
... Blackbody – is a hypothetical body that is a perfect absorber and emitter of EMR C spectrum – consists of a continuous range of frequencies w/o either bright or dark lines, appearing as a continuous range of colours E spectrum – consists of only radiation at a number of discrete wavelengths, appeari ...
Friday, April 26
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.