Temperature
... • Ionized gases at a star’s surface absorb specific frequencies of light. – Dark lines in a star’s spectrum ...
... • Ionized gases at a star’s surface absorb specific frequencies of light. – Dark lines in a star’s spectrum ...
Astrophysics 11 - HR Diagram
... • But AQA seem to prefer the absolute magnitude scale going from -15 to 10. ...
... • But AQA seem to prefer the absolute magnitude scale going from -15 to 10. ...
PPT file
... These stars consume their fuel faster and become red giants (they last for only 7 billion years) ...
... These stars consume their fuel faster and become red giants (they last for only 7 billion years) ...
Structure of the Sun, our nearest star
... ___________________. This reaction is called the “Triple-Alpha Process” ...
... ___________________. This reaction is called the “Triple-Alpha Process” ...
The life cycle of the Sun – HR Diagram
... increase with temperature) . High thermal conductivity of degenerate electron gas allows burning to spread quickly through the core. The increase in temperature does not cause an increase in pressure, and so the heat energy increases the rate of the triple alpha process generating more energy, furth ...
... increase with temperature) . High thermal conductivity of degenerate electron gas allows burning to spread quickly through the core. The increase in temperature does not cause an increase in pressure, and so the heat energy increases the rate of the triple alpha process generating more energy, furth ...
The Life of a Star - Department of Physics and Astronomy
... • “OK stellar recruits, it’s time to learn what’s really in store for you! I know that before you signed up to be a massive star you read the fancy brochures that talked about how brightly you’d be shining and how you’d be visible from halfway across the galaxy. But you mo-rons must not have bothere ...
... • “OK stellar recruits, it’s time to learn what’s really in store for you! I know that before you signed up to be a massive star you read the fancy brochures that talked about how brightly you’d be shining and how you’d be visible from halfway across the galaxy. But you mo-rons must not have bothere ...
HR DIAGRAM ACTIVITY
... 12. If you know a star’s color, you can determine its _________________ 13. (circle one) HOT or COLD stars have a shorter life span. 14. In the MAIN SEQUENCE, what color are the most massive stars? __________ In the MAIN SEQUENCE, what color are the least massive stars? __________ 15. You have disco ...
... 12. If you know a star’s color, you can determine its _________________ 13. (circle one) HOT or COLD stars have a shorter life span. 14. In the MAIN SEQUENCE, what color are the most massive stars? __________ In the MAIN SEQUENCE, what color are the least massive stars? __________ 15. You have disco ...
Chap. 02
... For a degenerate gas, the ignition of helium burning will heat the gas, but do not cause expand The increased temperature makes the reaction go faster, which further heats the gas, which makes the reaction goes faster. This cycle of explosive nuclear reaction continues until temperature is high enou ...
... For a degenerate gas, the ignition of helium burning will heat the gas, but do not cause expand The increased temperature makes the reaction go faster, which further heats the gas, which makes the reaction goes faster. This cycle of explosive nuclear reaction continues until temperature is high enou ...
The Mass-Luminosity Relationship and Stellar Lifetimes
... • Our intuition would seem to say that since big stars have a lot more fuel to consume, they should last a lot longer than smaller stars. • It doesn’t work this way, however. If the luminosity of a star increases with the 4th power of the mass, that means that the star is producing energy and using ...
... • Our intuition would seem to say that since big stars have a lot more fuel to consume, they should last a lot longer than smaller stars. • It doesn’t work this way, however. If the luminosity of a star increases with the 4th power of the mass, that means that the star is producing energy and using ...
Weathering, Erosion and Mass Movement
... Fusion is combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combining to form a helium nucleus. ...
... Fusion is combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combining to form a helium nucleus. ...
S03 from fusion to all the elements.notebook
... massenergy relationship, ________ the missing mass is converted to _________. ...
... massenergy relationship, ________ the missing mass is converted to _________. ...
KEY Unit 10‐11 Test Review: Characteristics of the Universe
... from Earth. Barnard‛s Star, on the other hand, is relatively close but is not visible to the unaided eye. This can be explained due to a DIFFERENCE in … ...
... from Earth. Barnard‛s Star, on the other hand, is relatively close but is not visible to the unaided eye. This can be explained due to a DIFFERENCE in … ...
Astronomy
... closer together As the distance decreases, gravitational forces increase Forms a “protostar.” The first stage in a star’s life. ...
... closer together As the distance decreases, gravitational forces increase Forms a “protostar.” The first stage in a star’s life. ...
Midterm 3 Review Sessions Two choices:
... Cooler regions where lines of force enter/leave surface. ...
... Cooler regions where lines of force enter/leave surface. ...
characteristics of stars
... close even though they are separated by large distance. Most of the stars outside the bulge are arranged in long ____________, called _________ which curve around the bulge. The entire Milky Way rotates around this bulge. The Milky Way Galaxy is called a ____________galaxy because of its circular, s ...
... close even though they are separated by large distance. Most of the stars outside the bulge are arranged in long ____________, called _________ which curve around the bulge. The entire Milky Way rotates around this bulge. The Milky Way Galaxy is called a ____________galaxy because of its circular, s ...
H-R diagram worksheet
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
Earth Science 25.2B : Stellar Evolution
... chemical elements beyond helium in the periodic table of elements. The process that produces chemical elements inside stars is called ...
... chemical elements beyond helium in the periodic table of elements. The process that produces chemical elements inside stars is called ...
Chapter 20 The Universe
... Galaxy- large grouping of stars -our solar system is part of Milky Way Galaxy - what we see as the Milky Way is only the edge ...
... Galaxy- large grouping of stars -our solar system is part of Milky Way Galaxy - what we see as the Milky Way is only the edge ...
Document
... neutrons worth of 2-3 solar masses. Some neutron stars spin rapidly and are detectable via their magnetic field direction. These are known as pulsars. 12. Even more massive stars can collapse to form a black hole– the gravity is so high that even the pressure from degenerate neutrons can not balance ...
... neutrons worth of 2-3 solar masses. Some neutron stars spin rapidly and are detectable via their magnetic field direction. These are known as pulsars. 12. Even more massive stars can collapse to form a black hole– the gravity is so high that even the pressure from degenerate neutrons can not balance ...
How Do Astronomers Measure the Brightness of a Star?
... vertical axis and temp (or spectral type) on the horizontal axis Sometimes the y axis is luminosity ...
... vertical axis and temp (or spectral type) on the horizontal axis Sometimes the y axis is luminosity ...
Life Cycle of Stars Powerpoint
... but is the size of Earth, it is one million times as dense as the sun. When a white dwarf runs out of fuel and energy it becomes a black dwarf. • A black dwarf has stopped glowing because fusion has stopped. It is a “dead” star, not the Death Star that is ...
... but is the size of Earth, it is one million times as dense as the sun. When a white dwarf runs out of fuel and energy it becomes a black dwarf. • A black dwarf has stopped glowing because fusion has stopped. It is a “dead” star, not the Death Star that is ...
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.