Notes
... E. _________________________ holds the solar system together 1. We usually think of gravity as the ____________________ that pulls us to the Earth. 2. True definition of gravity is the attractive force between ____________. 3. The more _________ an object has the ________ its gravitational pull. a. ...
... E. _________________________ holds the solar system together 1. We usually think of gravity as the ____________________ that pulls us to the Earth. 2. True definition of gravity is the attractive force between ____________. 3. The more _________ an object has the ________ its gravitational pull. a. ...
Document
... • Stars don’t live forever. Stars expand as it grows old. After the hydrogen (fuel) is used up, the star will begin to die. The core contracts and the outer layers expand, cool, and become less bright. It then becomes a red giant star. • Helium is now being used, and the core begins to shrink, and o ...
... • Stars don’t live forever. Stars expand as it grows old. After the hydrogen (fuel) is used up, the star will begin to die. The core contracts and the outer layers expand, cool, and become less bright. It then becomes a red giant star. • Helium is now being used, and the core begins to shrink, and o ...
The Hot-plate Model of a Star Model of Stars— 3 Oct
... hot-plate get to my hand? What are two ways to make a hot plate produce more energy per second? (The same question applies to a star: What are two ways to make a star brighter or more luminous?) What can I do to make the same hot-plate at the same setting burn my hand and not burn my hand? ...
... hot-plate get to my hand? What are two ways to make a hot plate produce more energy per second? (The same question applies to a star: What are two ways to make a star brighter or more luminous?) What can I do to make the same hot-plate at the same setting burn my hand and not burn my hand? ...
Stellar Spire in the Eagle Nebula
... and higher energies and frequencies than visible light. UV light is lower in frequency than X-rays. Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) ...
... and higher energies and frequencies than visible light. UV light is lower in frequency than X-rays. Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) ...
Unit 1
... – Instability comes from partial absorption of radiation in the interior of the star • Helium absorbs radiation, and the outer layers of the star get pushed away from core • As the star expands, the density decreases, letting photons escape • Outer layers head back inward toward core ...
... – Instability comes from partial absorption of radiation in the interior of the star • Helium absorbs radiation, and the outer layers of the star get pushed away from core • As the star expands, the density decreases, letting photons escape • Outer layers head back inward toward core ...
Life Cycle of a Star - Intervention Worksheet
... become later in its life; typically have the same ...
... become later in its life; typically have the same ...
Lecture 2
... much longer than that (it is about half way through its 10 billion year life) because it gets energy from nuclear reactions in its core, but when this source runs it will contract to become a white dwarf. It is the same for all other stars and in fact the more massive ones have much shorter lives wh ...
... much longer than that (it is about half way through its 10 billion year life) because it gets energy from nuclear reactions in its core, but when this source runs it will contract to become a white dwarf. It is the same for all other stars and in fact the more massive ones have much shorter lives wh ...
Stars
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
Apparent magnitude is the brightness of a star as it appears
... Apparent magnitude is the brightness of a star as it appears from Earth. This brightness depends partly on how far away the star is. Absolute magnitude describes the actual brightness of a star without considering its distance from the observer. The absolute magnitude of stars is measured on a Scale ...
... Apparent magnitude is the brightness of a star as it appears from Earth. This brightness depends partly on how far away the star is. Absolute magnitude describes the actual brightness of a star without considering its distance from the observer. The absolute magnitude of stars is measured on a Scale ...
Stellar Evolution
... and diameter. In fact, astronomers have discovered that the mass and the composition (makeup) of a star determine nearly all its other properties. ...
... and diameter. In fact, astronomers have discovered that the mass and the composition (makeup) of a star determine nearly all its other properties. ...
The Life Cycles of Stars
... star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more ...
... star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more ...
Components of the Milky Way
... • Giant molecular cloud forms a whole cluster of stars, may have mass of 106 Msun, size ~10 pc = 3 x 1019 cm • Molecular cloud core of a few Solar masses, perhaps 0.1 pc in size, forms one or (normally) a few stars. Estimate the characteristic time scales for these structures. ...
... • Giant molecular cloud forms a whole cluster of stars, may have mass of 106 Msun, size ~10 pc = 3 x 1019 cm • Molecular cloud core of a few Solar masses, perhaps 0.1 pc in size, forms one or (normally) a few stars. Estimate the characteristic time scales for these structures. ...
CMC The Universe – Pics of the day 1. Neutron Star A Neutron Star
... A black hole is formed when a massive star collapse in its cycle life. Then ...
... A black hole is formed when a massive star collapse in its cycle life. Then ...
The Mass-Luminosity Relationship and Stellar Lifetimes
... 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 its fuel at the same faster rate. ...
... 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 its fuel at the same faster rate. ...
Life Cycle of Stars
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
Lecture 15 - Deaths of Stars, Supernovae
... • Star burns up rest of hydrogen • Nothing remains but degenerate core of Oxygen and Carbon • “White dwarf” cools but does not contract because core is degenerate • No energy from fusion, no energy from gravitational contraction • White dwarf slowly fades away… ...
... • Star burns up rest of hydrogen • Nothing remains but degenerate core of Oxygen and Carbon • “White dwarf” cools but does not contract because core is degenerate • No energy from fusion, no energy from gravitational contraction • White dwarf slowly fades away… ...
Mark scheme for Support Worksheet – Topic E, Worksheet 1
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
Midterm 3 Review Sessions Two choices:
... • The Sun is a gas. • The Sun is neither contracting nor expanding. • Each point inside the Sun stays at a fixed temperature. • How energy generation rate depends on density, temperature, composition. • How energy is carried outwards. For every point in the Sun, we can then compute: • temperature • ...
... • The Sun is a gas. • The Sun is neither contracting nor expanding. • Each point inside the Sun stays at a fixed temperature. • How energy generation rate depends on density, temperature, composition. • How energy is carried outwards. For every point in the Sun, we can then compute: • temperature • ...
Life Cycle of Stars
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
The Life of a Star - Department of Physics and Astronomy
... moving more rapidly than average will escape, or leave the cluster • A stellar association is a group of newborn stars that are moving apart so rapidly that their gravitational attraction for one another cannot pull them into orbit about one another ...
... moving more rapidly than average will escape, or leave the cluster • A stellar association is a group of newborn stars that are moving apart so rapidly that their gravitational attraction for one another cannot pull them into orbit about one another ...
Learning Objectives Weeks 9-11 . 1. Know that star birth can begin
... 16. Explosive thermonuclear processes on white dwarfs and neutron stars produce novae and bursters. Novae and thermonuclear supernovae both occur in close binary systems with a white dwarf, but a while a nova can recur a supernova is a one-shot event. 17. Like a white dwarf, a neutron star has an u ...
... 16. Explosive thermonuclear processes on white dwarfs and neutron stars produce novae and bursters. Novae and thermonuclear supernovae both occur in close binary systems with a white dwarf, but a while a nova can recur a supernova is a one-shot event. 17. Like a white dwarf, a neutron star has an u ...
SNC1PL Celestial Objects and Constellations
... consistent patterns in the night sky. The IAU (International Astronomical Union) recognizes 88 constellations, but only 20 are truly prominent and may be easily identified ...
... consistent patterns in the night sky. The IAU (International Astronomical Union) recognizes 88 constellations, but only 20 are truly prominent and may be easily identified ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.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.