Star Life Cycle – Web Activity
... For today’s activity, you will need to visit http://aspire.cosmic-ray.org/Labs/StarLife/starlife_main.html Read the first page (don’t click on any of the “Table of Contents” items) and click on the arrow in the bottom right corner when you are finished. Below you will find questions and directions t ...
... For today’s activity, you will need to visit http://aspire.cosmic-ray.org/Labs/StarLife/starlife_main.html Read the first page (don’t click on any of the “Table of Contents” items) and click on the arrow in the bottom right corner when you are finished. Below you will find questions and directions t ...
No Slide Title
... • Some supernovas form neutron stars and black holes. – If the core that remains after a supernova has a mass of 1.4 to 3 solar masses, the remnant can become a neutron star. – If the leftover core has a mass that is greater than three solar masses, it will collapse to form a black hole. • black hol ...
... • Some supernovas form neutron stars and black holes. – If the core that remains after a supernova has a mass of 1.4 to 3 solar masses, the remnant can become a neutron star. – If the leftover core has a mass that is greater than three solar masses, it will collapse to form a black hole. • black hol ...
Mapping the Stars
... • What can a star become in this stage? • Red giant- a star that expands and cools once it uses all of its hydrogen. • What happens to the center of the star? • It shrinks due to the loss of hydrogen. • How big can red giants and supergiants become? • Red giants 10 or more times bigger than the sun ...
... • What can a star become in this stage? • Red giant- a star that expands and cools once it uses all of its hydrogen. • What happens to the center of the star? • It shrinks due to the loss of hydrogen. • How big can red giants and supergiants become? • Red giants 10 or more times bigger than the sun ...
Stars
... extremely massive. Stars in the Milky Way orbit around an unseen central object. Analysis of the orbital velocities of the stars about the center of the galaxy (using Kepler’s 3rd law) imply a mass of 2.6106 solar masses inside a volume 0.03 light years in diameter. It is impossible to pack stars t ...
... extremely massive. Stars in the Milky Way orbit around an unseen central object. Analysis of the orbital velocities of the stars about the center of the galaxy (using Kepler’s 3rd law) imply a mass of 2.6106 solar masses inside a volume 0.03 light years in diameter. It is impossible to pack stars t ...
Stellar Evolution of Single Stars
... Stellar Evolution of Single Stars Stellar evolution can be divided into 3 distinct phases: 1)Pre-main sequence evolution: a relatively short (~ 107-8 yrs) phase, but involving many complex processes. An active research area. 2)Main sequence phase: the longest phase of a star’s life ~ 1010 yrs for th ...
... Stellar Evolution of Single Stars Stellar evolution can be divided into 3 distinct phases: 1)Pre-main sequence evolution: a relatively short (~ 107-8 yrs) phase, but involving many complex processes. An active research area. 2)Main sequence phase: the longest phase of a star’s life ~ 1010 yrs for th ...
Powerpoint Presentation (large file)
... luminosity for main-sequence stars • The greater the mass of a main-sequence star, the greater its luminosity (and also the greater its radius and surface ...
... luminosity for main-sequence stars • The greater the mass of a main-sequence star, the greater its luminosity (and also the greater its radius and surface ...
ILÍDIO LOPES ()
... The κ-mechanism acts like an heat engine, converting thermal into mechanical energy. The stochastic driving is the main mechanism acting in sun-like stars and thus particularly important for our work. Here, the modes are driven stochastically by the turbulence of the subsurface convective zone. ...
... The κ-mechanism acts like an heat engine, converting thermal into mechanical energy. The stochastic driving is the main mechanism acting in sun-like stars and thus particularly important for our work. Here, the modes are driven stochastically by the turbulence of the subsurface convective zone. ...
Chapter 11: Stars
... strength of their hydrogen lines: A strongest, B slightly weaker, and O for the weakest. She classified more than 10,000 stars, which Pickering published in 1890. Annie Jump Cannon joined Pickering’s group in 1896. Building on the work of Fleming and Antonia Maury, she realized that the spectral cla ...
... strength of their hydrogen lines: A strongest, B slightly weaker, and O for the weakest. She classified more than 10,000 stars, which Pickering published in 1890. Annie Jump Cannon joined Pickering’s group in 1896. Building on the work of Fleming and Antonia Maury, she realized that the spectral cla ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... The reason for the changes between the classes was to do with some atoms becoming ionised at various temperature and at cooler temperature the light may not have sufficient energy to excite the atoms to create spectral lines. This meant the temperature of a star could be determined without worryin ...
... The reason for the changes between the classes was to do with some atoms becoming ionised at various temperature and at cooler temperature the light may not have sufficient energy to excite the atoms to create spectral lines. This meant the temperature of a star could be determined without worryin ...
Deducing Temperatures and Luminosities of Stars
... “Tools”, not “Problems” • If we can determine that 2 stars are identical, then their relative brightness translates to relative distances • Example: Sun vs. α Cen – spectra are very similar ⇒ temperatures, radii almost identical (T follows from Planck function, radius R can be deduced by other means ...
... “Tools”, not “Problems” • If we can determine that 2 stars are identical, then their relative brightness translates to relative distances • Example: Sun vs. α Cen – spectra are very similar ⇒ temperatures, radii almost identical (T follows from Planck function, radius R can be deduced by other means ...
02-02Stars_Part_One
... size, temperature, and distance. -1 is bright, 6 is dim •Absolute magnitude: Apparent magnitude at a distance of 10 parsecs. Factor of only size and temperature ...
... size, temperature, and distance. -1 is bright, 6 is dim •Absolute magnitude: Apparent magnitude at a distance of 10 parsecs. Factor of only size and temperature ...
Teaching ideas for Option E, Astrophysics
... questions about the Universe and its future evolution and eventual fate, questions that have been on man’s mind since ancient times. Unlike the ancients though, modern astrophysics has been able to provide precise methods that are helping answer these questions. Much of the success of modern astroph ...
... questions about the Universe and its future evolution and eventual fate, questions that have been on man’s mind since ancient times. Unlike the ancients though, modern astrophysics has been able to provide precise methods that are helping answer these questions. Much of the success of modern astroph ...
Stellar Evolution Guiding Questions Stars Evolve
... • Red giant becomes less luminous and smaller, but hotter. The core is in a steady state: – Temperature increases, core expands – Core expands, temperature decreases • Shell hydrogen fusion rate drops that lead to a lower ...
... • Red giant becomes less luminous and smaller, but hotter. The core is in a steady state: – Temperature increases, core expands – Core expands, temperature decreases • Shell hydrogen fusion rate drops that lead to a lower ...
Handout Life of Stars
... will suddenly and catastrophically collapse. The final collapse of a massive star under its own gravity happens incredibly quickly: in a thousandth of a second it can shrink from thousands of kilometres across to a ball of ultra-condensed matter just a few kilometres across. This rapid collapse resu ...
... will suddenly and catastrophically collapse. The final collapse of a massive star under its own gravity happens incredibly quickly: in a thousandth of a second it can shrink from thousands of kilometres across to a ball of ultra-condensed matter just a few kilometres across. This rapid collapse resu ...
M = 5.5 - The Millstone
... Case 1 Stars = 1 Solar Mass -> Red Giant -> White dwarf Stars such as our Sun move off the main sequence and enter the red giant branch (RGB), when the core hydrogen is exhausted. With no thermonuclear fusion in the core, the star contracts . An outer shell of hydrogen continues to burn and the radi ...
... Case 1 Stars = 1 Solar Mass -> Red Giant -> White dwarf Stars such as our Sun move off the main sequence and enter the red giant branch (RGB), when the core hydrogen is exhausted. With no thermonuclear fusion in the core, the star contracts . An outer shell of hydrogen continues to burn and the radi ...
Starlight and What it Tells Us
... The Heavens Are Not Changeless • The Stars Move – Most of our constellations would have been unrecognizable to Neanderthal Man ...
... The Heavens Are Not Changeless • The Stars Move – Most of our constellations would have been unrecognizable to Neanderthal Man ...
Lecture (Powerpoint)
... the mass of the Sun, or ~80 Jupiter masses) never ``turn on'' Central temperatures never get hot enough for nuclear burning to begin in earnest Nuclear burning is what powers the star through its life Star sits around as a brown dwarf – too big and hot to be a planet, too small and cold to be a real ...
... the mass of the Sun, or ~80 Jupiter masses) never ``turn on'' Central temperatures never get hot enough for nuclear burning to begin in earnest Nuclear burning is what powers the star through its life Star sits around as a brown dwarf – too big and hot to be a planet, too small and cold to be a real ...
White Dwarf Stars Near The Earth
... of a yellow-white dwarf than it is a white dwarf.) It takes a long time to cool off this much, probably nine billion years or more. The white dwarf known mostly by the rather anonymous catalog number GJ 440 is also a solo star. Its parent star was about double the mass of the Sun when it was young, ...
... of a yellow-white dwarf than it is a white dwarf.) It takes a long time to cool off this much, probably nine billion years or more. The white dwarf known mostly by the rather anonymous catalog number GJ 440 is also a solo star. Its parent star was about double the mass of the Sun when it was young, ...
Document
... • High Mass stars often times explode! • This spreads all of the elements Hydrogen through Iron (which makes up our planets and other new stars) and forms all elements after Iron (up to element 92). ...
... • High Mass stars often times explode! • This spreads all of the elements Hydrogen through Iron (which makes up our planets and other new stars) and forms all elements after Iron (up to element 92). ...
Star
A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, and the brightest stars gained proper names. Extensive catalogues of stars have been assembled by astronomers, which provide standardized star designations.For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime and, for some stars, by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, luminosity, and spectrum respectively. The total mass of a star is the principal determinant of its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung–Russell diagram (H–R diagram), allows the age and evolutionary state of a star to be determined.A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen fuel at the core is exhausted, a star with at least 0.4 times the mass of the Sun expands to become a red giant, in some cases fusing heavier elements at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or (if it is sufficiently massive) a black hole.Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution. Stars can form part of a much larger gravitationally bound structure, such as a star cluster or a galaxy.