Part 1—Stages of Human Life
... 1. Place the pictures in order from youngest to oldest. 2. Glue or tape the images to the paper. Draw in arrows showing the sequence. 3. Estimate the age of the person in the picture. 4. List some evidence of the person’s age. Be specific. 5. Do you have to see the entire life cycle of one person to ...
... 1. Place the pictures in order from youngest to oldest. 2. Glue or tape the images to the paper. Draw in arrows showing the sequence. 3. Estimate the age of the person in the picture. 4. List some evidence of the person’s age. Be specific. 5. Do you have to see the entire life cycle of one person to ...
Stars Unit 1-2: Stars
... in size, they vary even more in density! – Our sun has a density about 1.4 times greater than water. – Betelgeuse (don’t say it two more times!) is one-millionth the density of the sun. – Sirius is so dense, that one teaspoon of it would weigh more than a ton on earth! ...
... in size, they vary even more in density! – Our sun has a density about 1.4 times greater than water. – Betelgeuse (don’t say it two more times!) is one-millionth the density of the sun. – Sirius is so dense, that one teaspoon of it would weigh more than a ton on earth! ...
Document
... • Burns or converts H He via theromonuclear fusion in core • When hydrogen in the core is exhausted, converted into helium, the H-burning shell moves outward and the star expands • H-burning phase for another 5 billion years; inert He-core • Stars in H-burning phase are said to be Main Sequence st ...
... • Burns or converts H He via theromonuclear fusion in core • When hydrogen in the core is exhausted, converted into helium, the H-burning shell moves outward and the star expands • H-burning phase for another 5 billion years; inert He-core • Stars in H-burning phase are said to be Main Sequence st ...
V Example: our SUN (G2V)
... Denser stars with higher surface gravity will exhibit greater pressure broadening of spectral lines. Since the radius of a giant star is much greater than a dwarf star while their masses are roughly comparable, the gravity and thus the gas density and pressure on the surface of a giant star are much ...
... Denser stars with higher surface gravity will exhibit greater pressure broadening of spectral lines. Since the radius of a giant star is much greater than a dwarf star while their masses are roughly comparable, the gravity and thus the gas density and pressure on the surface of a giant star are much ...
The Hertzsprung – Russell Diagram Star Data Table
... Danish astronomer Ejnar Hertzsprung and American astronomer Henry Russell discovered a relationship between the brightness of a star and the surface temperature of a star. The graph of a star’s absolute magnitude versus its temperature is called an ...
... Danish astronomer Ejnar Hertzsprung and American astronomer Henry Russell discovered a relationship between the brightness of a star and the surface temperature of a star. The graph of a star’s absolute magnitude versus its temperature is called an ...
Compact Objects
... Chandrasehkar limit (1.4 Msun), electron degeneracy pressure cannot support it ...
... Chandrasehkar limit (1.4 Msun), electron degeneracy pressure cannot support it ...
Nebula - NICADD
... • A cool (10 K) nebula can be compressed by shock waves. – Shock waves from new stars and exploding stars. ...
... • A cool (10 K) nebula can be compressed by shock waves. – Shock waves from new stars and exploding stars. ...
- MrKowalik.com
... a. Use figure 3-3 How would you describe our solar system’s location in our galaxy? _____ ___________________________________________________________________ Stars 8. What is a star? _____________________________________________________ _______________________________________________________________ ...
... a. Use figure 3-3 How would you describe our solar system’s location in our galaxy? _____ ___________________________________________________________________ Stars 8. What is a star? _____________________________________________________ _______________________________________________________________ ...
!
... Cygnus X-1 is believed to be a black hole. Give two examples of how astronomers can (sometimes) determine whether an X-ray-emitting object is a neutron star or black hole. (2 points)! ...
... Cygnus X-1 is believed to be a black hole. Give two examples of how astronomers can (sometimes) determine whether an X-ray-emitting object is a neutron star or black hole. (2 points)! ...
The Death of High Mass Stars
... implying a mass of 15 Msun •Spectroscopic binary with P=5.6 days •Variability of 0.07mag implies orbit inclination of 30 degrees •Period combined with velocities from orbital parameters yields total system mass of ~23Msun •Mass of unseen companion: 8Msun (or at least more than 4Msun) •X-ray variabil ...
... implying a mass of 15 Msun •Spectroscopic binary with P=5.6 days •Variability of 0.07mag implies orbit inclination of 30 degrees •Period combined with velocities from orbital parameters yields total system mass of ~23Msun •Mass of unseen companion: 8Msun (or at least more than 4Msun) •X-ray variabil ...
Einstein
... supernovae become neutron stars • When stars between 4 and 9 times the mass of the Sun explode as supernovae, their remnant cores are highly compressed clumps of neutrons called neutron stars. – These tiny stars are much smaller than planet Earth in fact, are about the diameter of a large city (abou ...
... supernovae become neutron stars • When stars between 4 and 9 times the mass of the Sun explode as supernovae, their remnant cores are highly compressed clumps of neutrons called neutron stars. – These tiny stars are much smaller than planet Earth in fact, are about the diameter of a large city (abou ...
Stars - cmamath
... appear brighter than they really are (low apparent magnitude and high absolute magnitude.) Sun is a perfect example. High absolute magnitude (+5) and low apparent magnitude (-26.8) ...
... appear brighter than they really are (low apparent magnitude and high absolute magnitude.) Sun is a perfect example. High absolute magnitude (+5) and low apparent magnitude (-26.8) ...
Stars and the Main Sequence
... The generated heat will then exactly match the outgoing energy flow (luminosity) at any point in the star. Heat flows from hot to cold temperature gradient is required to carry the luminosity outward: Therefore T(r) and P(r) drop towards the surface (r) also drops ...
... The generated heat will then exactly match the outgoing energy flow (luminosity) at any point in the star. Heat flows from hot to cold temperature gradient is required to carry the luminosity outward: Therefore T(r) and P(r) drop towards the surface (r) also drops ...
Document
... the star per second) are the basic properties of a star • Magnitude: how bright the star appears; +1 was the brightest star, +2 was the next brightest star, +3 was the third brightest star • Absolute magnitude: takes into account distance and measures how bright a star would appear if they all were ...
... the star per second) are the basic properties of a star • Magnitude: how bright the star appears; +1 was the brightest star, +2 was the next brightest star, +3 was the third brightest star • Absolute magnitude: takes into account distance and measures how bright a star would appear if they all were ...
Stars Study Guide KEY
... *7. Which stars live the longest, high-mass or low-mass? Low Mass Stars live longer. Why? They have less self-gravity which means they burn through their fuel slower. 8. What will happen to our star, the Sun, at the end of its life? The sun will expand in the Red Giant phase, then will release its o ...
... *7. Which stars live the longest, high-mass or low-mass? Low Mass Stars live longer. Why? They have less self-gravity which means they burn through their fuel slower. 8. What will happen to our star, the Sun, at the end of its life? The sun will expand in the Red Giant phase, then will release its o ...
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.