Powerpoint
... Question 12 What type of atomic nuclei heavier than helium are most common, and why? ...
... Question 12 What type of atomic nuclei heavier than helium are most common, and why? ...
The Milky Way The Milky Way`s Neighbourhood
... Sun will emit in its entire ten billion year lifetime, as the guts of the star are blown outward into interstellar space. There are two general types of supernovae. A Type I supernova is the result of an existing, older white dwarf that gains enough mass to exceed the Chandrasekhar limit, causing a ...
... Sun will emit in its entire ten billion year lifetime, as the guts of the star are blown outward into interstellar space. There are two general types of supernovae. A Type I supernova is the result of an existing, older white dwarf that gains enough mass to exceed the Chandrasekhar limit, causing a ...
The Luminosity-Metallicity Relations for Star
... within a distance of 11 Mpc. Our goal is to fully characterize the star formation properties of complete samples of galaxies in the local universe. In particular, we are using this dataset to understand the importance of starbursts in dwarf galaxies. A preliminary analysis suggests that about 1 out ...
... within a distance of 11 Mpc. Our goal is to fully characterize the star formation properties of complete samples of galaxies in the local universe. In particular, we are using this dataset to understand the importance of starbursts in dwarf galaxies. A preliminary analysis suggests that about 1 out ...
The mass, temperature and distance of the white dwarf in V 471 Tauri
... and bright in the visible band. The optical pulsation ephemeris of Clemens et al. (1992) was very precise, allowing their phase to be recovered to within a fraction of a cycle for the ROSAT All-Sky Survey X-ray and EUV observations. Consequently, Barstow et al. (1992) were able to confirm that the X ...
... and bright in the visible band. The optical pulsation ephemeris of Clemens et al. (1992) was very precise, allowing their phase to be recovered to within a fraction of a cycle for the ROSAT All-Sky Survey X-ray and EUV observations. Consequently, Barstow et al. (1992) were able to confirm that the X ...
Stellar Evolution
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
Las enanas marrones y planetas aislados: quince años de un
... • First discoveries • Recent relevant results • Future of the substellar field • Summary ...
... • First discoveries • Recent relevant results • Future of the substellar field • Summary ...
To understand the deaths of stars and how it
... Electrons to the rescue! • It is humbling that to save this large star it takes something as small as an electron to save it. • At some point the density of the core gets to a MILLION times the density of water! • At this point the electrons are crammed so closely that they repel each other. • Whil ...
... Electrons to the rescue! • It is humbling that to save this large star it takes something as small as an electron to save it. • At some point the density of the core gets to a MILLION times the density of water! • At this point the electrons are crammed so closely that they repel each other. • Whil ...
ASTRONOMY 120: GALAXIES AND THE UNIVERSE HOMEWORK
... The total mass of the star is now M = 2.995M (the remaining 0.005M were converted into energy), of which 51.886% (=1.554/2.995) is Hydrogen, 47.112% (=1.411/2.995) is Helium and 1.002% (0.03/2.995) are heavy elements. Note that the use of four decimal places was used here to illustrate a slight ch ...
... The total mass of the star is now M = 2.995M (the remaining 0.005M were converted into energy), of which 51.886% (=1.554/2.995) is Hydrogen, 47.112% (=1.411/2.995) is Helium and 1.002% (0.03/2.995) are heavy elements. Note that the use of four decimal places was used here to illustrate a slight ch ...
Stellar Stability and the Chandrasekhar Limit
... They are known as the white dwarves. A white dwarf is an astronomical object which is produced when a low to medium mass star dies. These stars are not heavy enough to generate the core temperatures required to fuse carbon in nucleosynthesis reactions. After one has become a red giant during its he ...
... They are known as the white dwarves. A white dwarf is an astronomical object which is produced when a low to medium mass star dies. These stars are not heavy enough to generate the core temperatures required to fuse carbon in nucleosynthesis reactions. After one has become a red giant during its he ...
Hertzsprung-Russell Diagram—7 Oct Outline • Thermal radiation
... 2.9mm K 0.0005mm 500nm 5700K • For a person, T=273+37=310K. 2.9mm K 0.01mm 10μm 310K ...
... 2.9mm K 0.0005mm 500nm 5700K • For a person, T=273+37=310K. 2.9mm K 0.01mm 10μm 310K ...
Astronomy 82 - Problem Set #1
... degeneracy pressure instead of nuclear fusion. The maximum mass that can be supported by this pressure is 1.44 Msolar. (For each calculation, you can assume the star has uniform density.) a) If such a maximum mass white dwarf has a radius of 5400 km (slightly smaller than the Earth), what is its gra ...
... degeneracy pressure instead of nuclear fusion. The maximum mass that can be supported by this pressure is 1.44 Msolar. (For each calculation, you can assume the star has uniform density.) a) If such a maximum mass white dwarf has a radius of 5400 km (slightly smaller than the Earth), what is its gra ...
protostars and pre-main-sequence evolution.key
... using guessed central values for P, T, iterate until match with outer boundary conditions. ...
... using guessed central values for P, T, iterate until match with outer boundary conditions. ...
A detached white dwarf/M dwarf binary with an
... to the exact mass because of the form of the mass-radius relation, although it could be up to a factor of 2 smaller if the star is oversized for its mass, with the maximum size set by the Roche lobe. A further (K~ - K?-vv )/2c sin2 i = 0.1 km S-1 comes from the difference in transverse Doppler shift ...
... to the exact mass because of the form of the mass-radius relation, although it could be up to a factor of 2 smaller if the star is oversized for its mass, with the maximum size set by the Roche lobe. A further (K~ - K?-vv )/2c sin2 i = 0.1 km S-1 comes from the difference in transverse Doppler shift ...
printer-friendly sample test questions
... 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. expand into a red giant star. 9. Stellar black holes are remnants of very high-mass stars. These black holes will A. pull in matter from d ...
... 8. When fusion of hydrogen ceases in our Sun’s core, the Sun will A. explode as a supernova. B. collapse into white dwarf star. C. contract into a black hole. D. expand into a red giant star. 9. Stellar black holes are remnants of very high-mass stars. These black holes will A. pull in matter from d ...
RED DWARFS AND THE END OF THE MAIN SEQUENCE
... stars die off. Their contribution to the galactic luminosity is nearly compensated by the increase in luminosity of the smaller stars. The resulting latetime light curve for a large galaxy is thus remarkably constant. Figure 3 shows the expected light curve of our own galaxy under the assumption of ...
... stars die off. Their contribution to the galactic luminosity is nearly compensated by the increase in luminosity of the smaller stars. The resulting latetime light curve for a large galaxy is thus remarkably constant. Figure 3 shows the expected light curve of our own galaxy under the assumption of ...
Interacting binary stars Properties of some binary stars are
... Consequences of mass transfer: binary separation Do the stars in a binary get closer or move further apart as a result of mass transfer? • If separation declines - Roche lobes get smaller, so more mass transfer will occur. Normally this is unstable. • If separation increases - Roche lobes expand. T ...
... Consequences of mass transfer: binary separation Do the stars in a binary get closer or move further apart as a result of mass transfer? • If separation declines - Roche lobes get smaller, so more mass transfer will occur. Normally this is unstable. • If separation increases - Roche lobes expand. T ...
HAYASHI LIMIT
... To the right of the Hayashi limit no stars in a hydrostatic equilibrium can exist. ...
... To the right of the Hayashi limit no stars in a hydrostatic equilibrium can exist. ...
Incredible Shrinking Stars
... smaller than the stellar core. The stellar core was rotating (because it was part of a rotating star). When the core collapses, the rotation is concentrated (sort of) in the neutron. Consequently, tbe neutron star ends up spinning very rapidly 4. The interior of a neutron star consists of neutrons. ...
... smaller than the stellar core. The stellar core was rotating (because it was part of a rotating star). When the core collapses, the rotation is concentrated (sort of) in the neutron. Consequently, tbe neutron star ends up spinning very rapidly 4. The interior of a neutron star consists of neutrons. ...
File
... Small and medium stars become red giants and then _____ ____________. Their outer layers expand to become red giants. Eventually, the outer parts grow bigger still and drift out into space. The blue white hot core is left behind causing a white dwarf. When there is no more energy it become ...
... Small and medium stars become red giants and then _____ ____________. Their outer layers expand to become red giants. Eventually, the outer parts grow bigger still and drift out into space. The blue white hot core is left behind causing a white dwarf. When there is no more energy it become ...
Review: How does a star`s mass determine its life story?
... faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit). ...
... faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit). ...
Section 14
... A star can live billions of years this way; the Sun is believed to be approximately halfway through its estimated 10 billion-year life. However, it's lifetime is determined by its size at the outset--the larger the star, the shorter its life. However, the larger the star, the brighter it is. The Sun ...
... A star can live billions of years this way; the Sun is believed to be approximately halfway through its estimated 10 billion-year life. However, it's lifetime is determined by its size at the outset--the larger the star, the shorter its life. However, the larger the star, the brighter it is. The Sun ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of massive stars. The most massive stars become black holes when ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of massive stars. The most massive stars become black holes when ...