Galaxy3
... be set off in the density wave because the gas and dust are compressed. • After the interaction, there is continued star formation along the density wave as molecular clouds collide with the density wave and become compressed. ...
... be set off in the density wave because the gas and dust are compressed. • After the interaction, there is continued star formation along the density wave as molecular clouds collide with the density wave and become compressed. ...
Our Galaxy, the Milky Way Galaxy
... o Super bubbles – Around O/B associations About as thick as the Milky Way Galaxy itself! Super bubbles will grow (and move more ISM) when the O and B stars go supernova Remember, the gas is still moving around randomly! o The ISM is frothy (some parts are thicker/denser than others via randomn ...
... o Super bubbles – Around O/B associations About as thick as the Milky Way Galaxy itself! Super bubbles will grow (and move more ISM) when the O and B stars go supernova Remember, the gas is still moving around randomly! o The ISM is frothy (some parts are thicker/denser than others via randomn ...
Bluffer`s Guide to Orion
... sky. Sirius is the prominent star in the lower left, and part of Taurus can be seen at upper right. Diagram created with Starry Night software. years away and thirty light years across, and is the closest region of star formation to Earth. A lot of what proper astronomers know about how stars and pl ...
... sky. Sirius is the prominent star in the lower left, and part of Taurus can be seen at upper right. Diagram created with Starry Night software. years away and thirty light years across, and is the closest region of star formation to Earth. A lot of what proper astronomers know about how stars and pl ...
Lecture02-ASTA01 - University of Toronto
... you only how bright the star is as seen from Earth. • It doesn’t reveal anything about a star’s true power output – because the star’s distance is not known! • There is an “absolute magnitude scale” where we assign magnitudes that the object would have if placed at a certain distance known as 10 par ...
... you only how bright the star is as seen from Earth. • It doesn’t reveal anything about a star’s true power output – because the star’s distance is not known! • There is an “absolute magnitude scale” where we assign magnitudes that the object would have if placed at a certain distance known as 10 par ...
Stefan-Boltzmann Law Problems
... 1. A star with the same color as the Sun is found to produces a luminosity 81 times larger. What is its radius compared to the Sun? Since we are asked to compare this star to the Sun we will use a ratio technique that saves a lot of numerical work. Below I will decode the problem by writing out ht g ...
... 1. A star with the same color as the Sun is found to produces a luminosity 81 times larger. What is its radius compared to the Sun? Since we are asked to compare this star to the Sun we will use a ratio technique that saves a lot of numerical work. Below I will decode the problem by writing out ht g ...
FINAL STAGES OF MASSIVE STARS. SN EXPLOSION AND
... Explosion Mechanism Still Uncertain The explosive nucleosynthesis calculations for core collapse supernovae are still based on explosions induced by injecting an arbitrary amount of energy in a (also arbitrary) mass location of the presupernova model and then following the development of the blast w ...
... Explosion Mechanism Still Uncertain The explosive nucleosynthesis calculations for core collapse supernovae are still based on explosions induced by injecting an arbitrary amount of energy in a (also arbitrary) mass location of the presupernova model and then following the development of the blast w ...
Searching for Black Holes. Photometry in our Classrooms.
... components is a compact object probably a black hole or a neutron star, and the other component a „normal‟ star (usually a main sequence star or red giant) [5],[6]. The star usually orbits around the common center of mass gradually losing its mass towards the black hole or neutron star. Thus, the di ...
... components is a compact object probably a black hole or a neutron star, and the other component a „normal‟ star (usually a main sequence star or red giant) [5],[6]. The star usually orbits around the common center of mass gradually losing its mass towards the black hole or neutron star. Thus, the di ...
doc - Jnoodle
... The stars "near" us form the Milky Way, a galaxy containing ca 100 billion stars shaped like a disc with some spiral arms. The size of our galaxy is the order of magnitude 100 000 ly and it rotates around its center in ca 200 - 300 million years. Except start there is mostly thin interstellar matter ...
... The stars "near" us form the Milky Way, a galaxy containing ca 100 billion stars shaped like a disc with some spiral arms. The size of our galaxy is the order of magnitude 100 000 ly and it rotates around its center in ca 200 - 300 million years. Except start there is mostly thin interstellar matter ...
Our Star - U of L Class Index
... of mass, luminosity and temperature. It’s only special because it’s so close to us. The next nearest star is about ...
... of mass, luminosity and temperature. It’s only special because it’s so close to us. The next nearest star is about ...
THE UNIVERSE - - GRADE 9, UNIT 4 (4 weeks)
... 1. The formation of stars is described as stages of evolution. a. early in the formation of the universe, stars coalesced out of clouds of hydrogen and helium and clumped together by gravitational attraction into galaxies b. stars are classified by their color, size, luminosity and mass. c. Hertzspr ...
... 1. The formation of stars is described as stages of evolution. a. early in the formation of the universe, stars coalesced out of clouds of hydrogen and helium and clumped together by gravitational attraction into galaxies b. stars are classified by their color, size, luminosity and mass. c. Hertzspr ...
ASTRONOMY 5
... b) Although dark matter emits no visible light, it can be seen with radio telescopes, and such observations confirm that the halo of our Galaxy is full of this material. c) Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we s ...
... b) Although dark matter emits no visible light, it can be seen with radio telescopes, and such observations confirm that the halo of our Galaxy is full of this material. c) Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we s ...
Disks around low-mass stars in extreme environments
... only from core-collapse supernovae Must have been injected into the proto-solar nebula at most a few Myr after the formation of our Sun. Our solar system formed in an environment containing high-mass stars (M✶ > 30 M⊙) ...
... only from core-collapse supernovae Must have been injected into the proto-solar nebula at most a few Myr after the formation of our Sun. Our solar system formed in an environment containing high-mass stars (M✶ > 30 M⊙) ...
Measuring the mass of galaxies Luminous matter in a
... Rotation curves of other spiral galaxies Can also measure the rotation curve of other spiral galaxies Use the Doppler shift of spectral lines emitted by hydrogen gas to infer velocity of rotation same idea as for measuring redshifts ...
... Rotation curves of other spiral galaxies Can also measure the rotation curve of other spiral galaxies Use the Doppler shift of spectral lines emitted by hydrogen gas to infer velocity of rotation same idea as for measuring redshifts ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.