Stellar Evolution
... together to form helium in the core of a young star. Some older, bigger stars can either fuse helium to form other elements or no fusion ...
... together to form helium in the core of a young star. Some older, bigger stars can either fuse helium to form other elements or no fusion ...
Study Notes for Chapter 30:
... Hubble’s discovery that there was ____ shift in the spectra of galaxies lead to an understanding that the universe is ____. ...
... Hubble’s discovery that there was ____ shift in the spectra of galaxies lead to an understanding that the universe is ____. ...
Study Notes for Chapter 30:
... Hubble’s discovery that there was ____ shift in the spectra of galaxies lead to an understanding that the universe is ____. ...
... Hubble’s discovery that there was ____ shift in the spectra of galaxies lead to an understanding that the universe is ____. ...
The Birth of Stars
... enough that the dust is thick and gravity can collapse knots in these “molecular” clouds to make new stars. ...
... enough that the dust is thick and gravity can collapse knots in these “molecular” clouds to make new stars. ...
PowerPoint File
... • So, massive stars run out of fuel sooner. The more massive, the shorter their Main Sequence lifetime ...
... • So, massive stars run out of fuel sooner. The more massive, the shorter their Main Sequence lifetime ...
80.BrainPopLifeCycleStars
... ___________ of years. 2. They start out as clouds of gas and dust called __________ nurseries. The force of __________ within these clouds slowly pulls the particles together, causing dense clumps to form. 3. If the clump becomes large enough, the ____________ caused by gravity forms a __________, a ...
... ___________ of years. 2. They start out as clouds of gas and dust called __________ nurseries. The force of __________ within these clouds slowly pulls the particles together, causing dense clumps to form. 3. If the clump becomes large enough, the ____________ caused by gravity forms a __________, a ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... 2. The birthplaces of stars are dark, cool interstellar ______________. These nebulae are made up of ____________ and gases. For some reason, some nebulae become dense enough to begin to _______________. A shock wave from an ___________________ of a nearby star may trigger the contraction. Once the ...
... 2. The birthplaces of stars are dark, cool interstellar ______________. These nebulae are made up of ____________ and gases. For some reason, some nebulae become dense enough to begin to _______________. A shock wave from an ___________________ of a nearby star may trigger the contraction. Once the ...
The death of a star
... I will answer it by the following shortened version of the life of a star such as our Sun after it has reached the 'normal' star state. As far as expansion and contraction are concerned it all depends which part of the stellar cycle you are interested in. Both occur between the 'normal' state and th ...
... I will answer it by the following shortened version of the life of a star such as our Sun after it has reached the 'normal' star state. As far as expansion and contraction are concerned it all depends which part of the stellar cycle you are interested in. Both occur between the 'normal' state and th ...
Stellar Evolution
... fuse helium into carbon and oxygen. The core cannot get hot enough to fuse carbon and oxygen, so when the helium runs out, fusion stops. The outer layers of the star are blown off, and you are left with a “white dwarf” which slowly cools off and grows dim, becoming a brown dwarf. ...
... fuse helium into carbon and oxygen. The core cannot get hot enough to fuse carbon and oxygen, so when the helium runs out, fusion stops. The outer layers of the star are blown off, and you are left with a “white dwarf” which slowly cools off and grows dim, becoming a brown dwarf. ...
Self Assessment: Life Cycle of a Star
... a) the collapse of the iron core of an intermediate mass star b) the collapse of the iron core of a star with a mass greater than about six solar masses c) the collapse of a planetary nebula d) the collapse of the a star's core during the formation of a planetary nebula 4. The length of a star's l ...
... a) the collapse of the iron core of an intermediate mass star b) the collapse of the iron core of a star with a mass greater than about six solar masses c) the collapse of a planetary nebula d) the collapse of the a star's core during the formation of a planetary nebula 4. The length of a star's l ...
Study Notes for Integrated Science Astronomy Unit These notes will
... route of a stars life cycle is dependent on the mass of the star. There are common stages in all star life cycles: nebula, protostar, main sequence, and expansion after the hydrogen is nearly all fused into helium. There are also very different stages that differ the life cycle of large stars red su ...
... route of a stars life cycle is dependent on the mass of the star. There are common stages in all star life cycles: nebula, protostar, main sequence, and expansion after the hydrogen is nearly all fused into helium. There are also very different stages that differ the life cycle of large stars red su ...
Lecture 26 - Empyrean Quest Publishers
... 2. Molecular Clouds--H2 molecules--dense MC are star formation regions (stellar nurseries like Orion Nebula). ...
... 2. Molecular Clouds--H2 molecules--dense MC are star formation regions (stellar nurseries like Orion Nebula). ...
red giant
... • Helium flash goes off in shrinking degenerate core: horizontal branch star with He core burning • Double shell burning (H and He) yields red supergiant (RG II), blows off planetary nebula • Read 18.2 about white dwarfs formed at end of evolution of low-mass stars • Respond to discussion question p ...
... • Helium flash goes off in shrinking degenerate core: horizontal branch star with He core burning • Double shell burning (H and He) yields red supergiant (RG II), blows off planetary nebula • Read 18.2 about white dwarfs formed at end of evolution of low-mass stars • Respond to discussion question p ...
CMC The Universe – Pics of the day 1. Neutron Star A Neutron Star
... OpenOffice didn't let me upload the video here in the presentation, so I just could write the link ...
... OpenOffice didn't let me upload the video here in the presentation, so I just could write the link ...
Stars after the Main Sequence. Example: Betelgeuse (Alpha Orionis
... These compact cores exist….the white dwarf stars ...
... These compact cores exist….the white dwarf stars ...
Star Life Cycles Stellar Nebula
... As planetary nebula expands, remaining core glows white, but is much smaller than original star White Dwarf ...
... As planetary nebula expands, remaining core glows white, but is much smaller than original star White Dwarf ...
Stellar Notes
... details can you come up with for a Stellar Nursery, or better known as a Nebula? ...
... details can you come up with for a Stellar Nursery, or better known as a Nebula? ...
The Life Cycles of Stars
... the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage. At this stage, the star’s matte ...
... the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage. At this stage, the star’s matte ...
GLY 4045 Moons, Planets, and Meteors: An Introduction to
... Competency 3: Students will explain the dynamics of planetary orbits by: a. Diagramming both the 2 body and 3 body problems b. Discussing planetary perturbations and long-term stability of planetary orbits Competency 4: Students will summarize the effect of solar heat and energy in planetary atmosph ...
... Competency 3: Students will explain the dynamics of planetary orbits by: a. Diagramming both the 2 body and 3 body problems b. Discussing planetary perturbations and long-term stability of planetary orbits Competency 4: Students will summarize the effect of solar heat and energy in planetary atmosph ...
Evolution and the Big Bang, ET Life Lec. 6, Jan 18, 2002
... By about 3 min. after Big Bang all of the neutrons are bound into 4He nuclei which have two protons (Helium has Z=2) and 2 neutrons. Remaining protons are free to form Hydrogen (Z=1). Thus Universe was about 25% He and 75% H and little heavier elements (those with Z>2). ...
... By about 3 min. after Big Bang all of the neutrons are bound into 4He nuclei which have two protons (Helium has Z=2) and 2 neutrons. Remaining protons are free to form Hydrogen (Z=1). Thus Universe was about 25% He and 75% H and little heavier elements (those with Z>2). ...
HNRS 227 Lecture #2 Chapters 2 and 3
... Planetary Observations Planets formed at same time as Sun Planetary and satellite/ring systems are similar to remnants of dusty disks such as that seen about stars being born Planet composition dependent upon where it formed in solar system ...
... Planetary Observations Planets formed at same time as Sun Planetary and satellite/ring systems are similar to remnants of dusty disks such as that seen about stars being born Planet composition dependent upon where it formed in solar system ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.