Chemistry study guide 09
... Protons & neutrons both have a mass = 1 atomic mass Electrons have a mass of 1/2000 very tiny Atomic number is the number of protons in an atom atomic number/ number of protons atomic mass Atomic mass: this is the mass of the particles found in the nucleus/ always a decimal Mass number: the atom ...
... Protons & neutrons both have a mass = 1 atomic mass Electrons have a mass of 1/2000 very tiny Atomic number is the number of protons in an atom atomic number/ number of protons atomic mass Atomic mass: this is the mass of the particles found in the nucleus/ always a decimal Mass number: the atom ...
Star in a Box Worksheet - Beginning with solutions
... 1. What stages of their lives are the two stars in? Deneb is between the main sequence and the Hertzsprung Gap. Betelgeuse is between the Hertzsprung Gap and core helium burning. 2. How long does each star have to live? D eneb has about 1 million years left to live and Betelgeuse has about 400 th ...
... 1. What stages of their lives are the two stars in? Deneb is between the main sequence and the Hertzsprung Gap. Betelgeuse is between the Hertzsprung Gap and core helium burning. 2. How long does each star have to live? D eneb has about 1 million years left to live and Betelgeuse has about 400 th ...
Answers to Coursebook questions – Chapter E5
... A one solar mass star would evolve to become a red giant. As the star expands in size into the red giant stage, nuclear reactions inside the core of the star are able to produce heavier elements than helium because the temperature of the core is sufficiently high. The red giant star will explode as ...
... A one solar mass star would evolve to become a red giant. As the star expands in size into the red giant stage, nuclear reactions inside the core of the star are able to produce heavier elements than helium because the temperature of the core is sufficiently high. The red giant star will explode as ...
The Magic of Star Dust - Exploring Exotic Nuclei
... with a big bang that created a soup of objects, among which were the massive ones called nucleons. The soup contained both positively charged nucleons called ‘protons’ and electrically neutral ones called ‘neutrons’. As the universe cooled and expanded the hadrons coalesced together to form more com ...
... with a big bang that created a soup of objects, among which were the massive ones called nucleons. The soup contained both positively charged nucleons called ‘protons’ and electrically neutral ones called ‘neutrons’. As the universe cooled and expanded the hadrons coalesced together to form more com ...
The Life of a Star
... When the core of a medium mass star reaches 1.0 x 106°C, helium fusion begins in the core (secondary fusion). Once all fusion reactions stop, the star throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is call ...
... When the core of a medium mass star reaches 1.0 x 106°C, helium fusion begins in the core (secondary fusion). Once all fusion reactions stop, the star throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is call ...
wk9 (part 1)
... • The Zero Age Main Sequence (ZAMS) represents the onset or start of nuclear burning (fusion) • The properties of a star on the ZAMS are primarily determined by its mass, somewhat dependent on chemical composition (fraction of He and heavier elements) • The classification of stars in an HR diagram b ...
... • The Zero Age Main Sequence (ZAMS) represents the onset or start of nuclear burning (fusion) • The properties of a star on the ZAMS are primarily determined by its mass, somewhat dependent on chemical composition (fraction of He and heavier elements) • The classification of stars in an HR diagram b ...
astronomy - Mr. Barnard
... ____3. The probable fate of our sun is (1) to become a black hole (2) to shrink to a white dwarf then eventually expand to a red giant (3) to expand as a red giant, undergo a nova outburst and end as a white dwarf (4) become hotter and expand into a blue supergiant ____4. Eventually the sun is expec ...
... ____3. The probable fate of our sun is (1) to become a black hole (2) to shrink to a white dwarf then eventually expand to a red giant (3) to expand as a red giant, undergo a nova outburst and end as a white dwarf (4) become hotter and expand into a blue supergiant ____4. Eventually the sun is expec ...
The_Birth_of_a_Star
... • If the star is very large, it burns through the hydrogen quickly; helium fuses to make carbon, and as the helium is exhausted the collapse of the core generates enough energy to fuse the carbon forming iron. • Eventually the star collapses, as the electrons are trapped inside the core, forming ne ...
... • If the star is very large, it burns through the hydrogen quickly; helium fuses to make carbon, and as the helium is exhausted the collapse of the core generates enough energy to fuse the carbon forming iron. • Eventually the star collapses, as the electrons are trapped inside the core, forming ne ...
14-1 Reading Questions: Neutron Stars
... 1. A neutron star, containing a little more than _________ solar mass, compressed to a radius of about __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a __________________ ...
... 1. A neutron star, containing a little more than _________ solar mass, compressed to a radius of about __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a __________________ ...
Final Review Sheet
... Hydrogen continues to burn in an overlying shell that is super hot because of the contraction of the helium core to higher density More energy is generated by the hydrogen shell than is required to stay on the main sequence. If star was convective (eg., M = 0.5) its luminosity increases immediately. ...
... Hydrogen continues to burn in an overlying shell that is super hot because of the contraction of the helium core to higher density More energy is generated by the hydrogen shell than is required to stay on the main sequence. If star was convective (eg., M = 0.5) its luminosity increases immediately. ...
Lecture Notes – Stars
... In most cases, the masses are consistent with neutron stars. In a few cases the masses are much higher, suggesting a black hole. Best known example is Cygnus X-1 which has an invisible companion with a mass of 8 M . SUPERNOVAE Massive stars are able to fuse elements up to Fe which absorbs rather th ...
... In most cases, the masses are consistent with neutron stars. In a few cases the masses are much higher, suggesting a black hole. Best known example is Cygnus X-1 which has an invisible companion with a mass of 8 M . SUPERNOVAE Massive stars are able to fuse elements up to Fe which absorbs rather th ...
S1E4 Extreme Stars
... What holds the white dwarf from collapsing? • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can d ...
... What holds the white dwarf from collapsing? • The resulting outward pressure which keeps the electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can d ...
Nuclear Physics and Radioactivity2
... At the beginning of the century (1900), not much was known about the atom. The electron was discovered by J.J. Thomson in 1897. Thomson did not know much was known about the electron and advanced the "plum pudding" model of the atom. The number of electrons contained in an atom could not be determin ...
... At the beginning of the century (1900), not much was known about the atom. The electron was discovered by J.J. Thomson in 1897. Thomson did not know much was known about the electron and advanced the "plum pudding" model of the atom. The number of electrons contained in an atom could not be determin ...
Review: How does a star`s mass determine its life story?
... C. Nothing: the directions would cancel each other out. ...
... C. Nothing: the directions would cancel each other out. ...
Powerpoint of lecture 16
... isothermality, internal pressure gradients build up and core contraction slows to thermal timescale, with slow release of gravitational energy • H-shell very T-sensitive – acts as thermostat: ...
... isothermality, internal pressure gradients build up and core contraction slows to thermal timescale, with slow release of gravitational energy • H-shell very T-sensitive – acts as thermostat: ...
Stars: Other Suns
... • Measure directly only with binary systems of stars (lots!) • Revolve around center of mass • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
... • Measure directly only with binary systems of stars (lots!) • Revolve around center of mass • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.