Star Formation
... Star formation is triggered when an interstellar cloud is compressed by a shock wave ...
... Star formation is triggered when an interstellar cloud is compressed by a shock wave ...
Midterm II Jeopardy
... $1600 - This prevents collapse of the star at the center of a planetary nebula (Electron degeneracy pressure) Sharp Things (stars): $400 - This “failed star” did not have a high enough T to sustain long-term fusion (BD) $800 - An “HR diagram” is a plot of which two quantities (T(or spectral type) vs ...
... $1600 - This prevents collapse of the star at the center of a planetary nebula (Electron degeneracy pressure) Sharp Things (stars): $400 - This “failed star” did not have a high enough T to sustain long-term fusion (BD) $800 - An “HR diagram” is a plot of which two quantities (T(or spectral type) vs ...
Ourdraft
... Young Stars in IC 2118 We are studying a nebula (cloud of gas and dust) called Interstellar Cloud 2118, or the Witch Head Nebula, that is being excited by a young, very hot star called Rigel. Because Rigel is so energetic, it sends off shock waves that hit the nebula, compressing some of the gas (at ...
... Young Stars in IC 2118 We are studying a nebula (cloud of gas and dust) called Interstellar Cloud 2118, or the Witch Head Nebula, that is being excited by a young, very hot star called Rigel. Because Rigel is so energetic, it sends off shock waves that hit the nebula, compressing some of the gas (at ...
Supernovae, Neutron Stars, Black Holes
... in which the Sun and planets formed) contained radioactive isotopes with half-lives so short that they no longer exist. These include isotopes with very short half-lives, such as calcium-41, 41Ca, (100,000 years) and aluminum-26, 26Al, (740,000 years), and those with longer half-lives such as pluton ...
... in which the Sun and planets formed) contained radioactive isotopes with half-lives so short that they no longer exist. These include isotopes with very short half-lives, such as calcium-41, 41Ca, (100,000 years) and aluminum-26, 26Al, (740,000 years), and those with longer half-lives such as pluton ...
File
... huge size mean low temperature... it is now a ______ ________. The outer layer of gas gets blown off producing a cloud of gas called a ___________ ______________ leaving a hot, dense core...it is now a ________ __________. the white dwarf eventually cools into a _________ __________. MASSIVE ...
... huge size mean low temperature... it is now a ______ ________. The outer layer of gas gets blown off producing a cloud of gas called a ___________ ______________ leaving a hot, dense core...it is now a ________ __________. the white dwarf eventually cools into a _________ __________. MASSIVE ...
The Mass of the Galaxy - University of California, Berkeley
... In other galaxies, the arms are easy to see because their ISM does not hide optical diagnostics from us. There are always only a few arms (often 2), and they are never too tightly wound. O & B stars ...
... In other galaxies, the arms are easy to see because their ISM does not hide optical diagnostics from us. There are always only a few arms (often 2), and they are never too tightly wound. O & B stars ...
Loving The Universe
... the universe is all of a piece and that it began as a single seed smaller than an atom. And in a very real sense, you and I were there. Every scrap of matter and energy in our blood and bones, and in the synapses of our thoughts can trace its lineage back to the origin of the universe ... as the Kor ...
... the universe is all of a piece and that it began as a single seed smaller than an atom. And in a very real sense, you and I were there. Every scrap of matter and energy in our blood and bones, and in the synapses of our thoughts can trace its lineage back to the origin of the universe ... as the Kor ...
Life Cycle of the Stars
... A Star is Born • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the d ...
... A Star is Born • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the d ...
Quiz Questions
... 4. Energy is produced at the center of the Sun. By the time it reaches our eyes, it has been transported by A. conduction (by collisions between particles) D. A and B B. convection (by bulk motion of matter) E. B and C C. radiation (by photons) 5. If we know the true luminosity (Watts) of a star and ...
... 4. Energy is produced at the center of the Sun. By the time it reaches our eyes, it has been transported by A. conduction (by collisions between particles) D. A and B B. convection (by bulk motion of matter) E. B and C C. radiation (by photons) 5. If we know the true luminosity (Watts) of a star and ...
Chapter 7 Vocabulary212
... 1. Spectroscope- used to study star’s characteristics by spreading light into different wavelengths 2. Nuclear fusion- nuclei of several atoms combine to form on large nucleus 3. astronomical unit- average distance between Earth and Sun (150 million km) 4. light year- distance light travels in 1 yea ...
... 1. Spectroscope- used to study star’s characteristics by spreading light into different wavelengths 2. Nuclear fusion- nuclei of several atoms combine to form on large nucleus 3. astronomical unit- average distance between Earth and Sun (150 million km) 4. light year- distance light travels in 1 yea ...
2.5.2 development of a star
... During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in the plastic of the balloon. In the star it is known ...
... During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in the plastic of the balloon. In the star it is known ...
Ch. 19 (Starbirth)
... This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permit ...
... This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permit ...
Star Fromation and ISM
... the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, but more quickly • Less massive stars form m ...
... the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, but more quickly • Less massive stars form m ...
20.1 Notes
... own gravity and rebounds with a shock wave that violently blows the stars outer layers from the core. This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very den ...
... own gravity and rebounds with a shock wave that violently blows the stars outer layers from the core. This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very den ...
Video review
... 2. A collapsing gas cloud (nebula) that form a star system increases its rotation rate because of the conservation of _________________ momentum. 3. The protostar is the early stage of a star that forms at the ____________ of the collapsing gas cloud. 4. The Sun formed in the center of the nebular c ...
... 2. A collapsing gas cloud (nebula) that form a star system increases its rotation rate because of the conservation of _________________ momentum. 3. The protostar is the early stage of a star that forms at the ____________ of the collapsing gas cloud. 4. The Sun formed in the center of the nebular c ...
PHYSICS 015
... Note that the material in the nebula is raw star stuff – not the products of the nuclear reactions deep within the core! It is almost pure H + He. The escaping material eventually merges into the interstellar medium, and is available to be used in other stars that may form later. ...
... Note that the material in the nebula is raw star stuff – not the products of the nuclear reactions deep within the core! It is almost pure H + He. The escaping material eventually merges into the interstellar medium, and is available to be used in other stars that may form later. ...
potters powerpoint
... • Stars shine because of the heat they make. The heat of a star reaches about 16million degrees Celsius. A grain of sand that hot could kill someone 150km away. ...
... • Stars shine because of the heat they make. The heat of a star reaches about 16million degrees Celsius. A grain of sand that hot could kill someone 150km away. ...
Chapter11
... contracting star and gives it stability? We can understand this phenomenon because we understand some of the basic laws of physics. ...
... contracting star and gives it stability? We can understand this phenomenon because we understand some of the basic laws of physics. ...
Today`s Powerpoint
... gas. Some collapse under their own gravity. Others may be more stable. Magnetic fields and rotation also have some influence. Gravity makes cloud want to collapse. ...
... gas. Some collapse under their own gravity. Others may be more stable. Magnetic fields and rotation also have some influence. Gravity makes cloud want to collapse. ...
Astronomy Powerpoint
... Life Cycle of a star • Begins as a cloud of gas • Core reaches 1 million C, energy is given off • When most of the hydrogen is used up, becomes a red giant • Depending on size, becomes a white dwarf or a supernova ...
... Life Cycle of a star • Begins as a cloud of gas • Core reaches 1 million C, energy is given off • When most of the hydrogen is used up, becomes a red giant • Depending on size, becomes a white dwarf or a supernova ...
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.