name - New York Science Teacher
... 10. -What spectral class of stars is the hottest? ____________________________ 11. -What spectral class of stars is the coolest? ____________________________ 12. - What spectral class is our sun? ____________________________ ...
... 10. -What spectral class of stars is the hottest? ____________________________ 11. -What spectral class of stars is the coolest? ____________________________ 12. - What spectral class is our sun? ____________________________ ...
Chapter 18 Study Guide
... White dwarf 9. What type of star has a low temperature but a high luminosity? (use H-R Diagram to determine) Red supergiant 10. According to the Hertzsprung-Russell diagram, what relationship exist between the brightness and temperature of a main sequence star? The Hertzsprung- Russell diagram shows ...
... White dwarf 9. What type of star has a low temperature but a high luminosity? (use H-R Diagram to determine) Red supergiant 10. According to the Hertzsprung-Russell diagram, what relationship exist between the brightness and temperature of a main sequence star? The Hertzsprung- Russell diagram shows ...
potters powerpoint
... Why do stars shine ? • 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. ...
... Why do stars shine ? • 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. ...
1 Ay 124 Winter 2014 – HOMEWORK #2 Problem 1
... Assume that stars have luminosities L ∝ M 4 . In parts (a) and (b) consider only stars more massive than 1M , whose lifetimes are shorter than the age of the galaxy. a) Find the slope x such that an observer in a homogeneous, isotropic region counts, at every apparent bolmetric magnitude, equal num ...
... Assume that stars have luminosities L ∝ M 4 . In parts (a) and (b) consider only stars more massive than 1M , whose lifetimes are shorter than the age of the galaxy. a) Find the slope x such that an observer in a homogeneous, isotropic region counts, at every apparent bolmetric magnitude, equal num ...
White Dwarf Stars After nuclear burning ceases, a post
... In theory, there are three mechanisms which can cause mechanical instability in a star. The ϵ mechanism: If the center of the star is compressed slightly, the nuclear reaction rates will go up, causing an increase in expansion. The expansion can then decrease the reaction rates, cool the central cor ...
... In theory, there are three mechanisms which can cause mechanical instability in a star. The ϵ mechanism: If the center of the star is compressed slightly, the nuclear reaction rates will go up, causing an increase in expansion. The expansion can then decrease the reaction rates, cool the central cor ...
www.NewYorkScienceTeacher.org/review
... shorter or longer, the observer can determine if the star is moving toward or away from Earth. These shifts are called blueshifts and redshifts. The larger the shift, the higher the speed of motion. The shifts in spectral lines can also be used to detect binary stars as they orbit around their cente ...
... shorter or longer, the observer can determine if the star is moving toward or away from Earth. These shifts are called blueshifts and redshifts. The larger the shift, the higher the speed of motion. The shifts in spectral lines can also be used to detect binary stars as they orbit around their cente ...
1: The scientific name for my field is astronomy
... 1: The scientific name for my field is Astronomy. 2: Chapters 20-22 in Earth Science deal with my field. 3: None of the chapters in the Science Interactions brown book are based on Astronomy. 4: Chapters 19-20 in the Science Interactions blue book are based on Astronomy. 5: Astronomers study anythin ...
... 1: The scientific name for my field is Astronomy. 2: Chapters 20-22 in Earth Science deal with my field. 3: None of the chapters in the Science Interactions brown book are based on Astronomy. 4: Chapters 19-20 in the Science Interactions blue book are based on Astronomy. 5: Astronomers study anythin ...
Lecture 11 - Stars and Atomic Spectra
... Classifying stars Photons Atomic structure Elements in stars Masses of stars Mass-luminosity relation ...
... Classifying stars Photons Atomic structure Elements in stars Masses of stars Mass-luminosity relation ...
Astronomy.Practice.Quiz3
... a. absolute magnitude and apparent magnitude b. temperature and absolute magnitude c. parallax and temperature d. apparent magnitude and parallax 11. The source of the Sun’s energy is ____. a. chemical burning b. nuclear fusion 12. What determines the final stages of a star’s life cycle? a. size b. ...
... a. absolute magnitude and apparent magnitude b. temperature and absolute magnitude c. parallax and temperature d. apparent magnitude and parallax 11. The source of the Sun’s energy is ____. a. chemical burning b. nuclear fusion 12. What determines the final stages of a star’s life cycle? a. size b. ...
Lecture 15, PPT version
... It’s only a matter of time before the star gets in trouble again… This time it’s CARBON ash that has sunk to the center (non-burning carbon core, surrounded by a shell of He burning, surrounded by a shell of H burning). ...
... It’s only a matter of time before the star gets in trouble again… This time it’s CARBON ash that has sunk to the center (non-burning carbon core, surrounded by a shell of He burning, surrounded by a shell of H burning). ...
Hertzsprung-Russell Diagram
... The main sequence is not really a line. The sun fits on the main sequence when it has a luminosity of 0.5 to 1.5 the actual luminosity. The reason is due to the age and composition of the star. ...
... The main sequence is not really a line. The sun fits on the main sequence when it has a luminosity of 0.5 to 1.5 the actual luminosity. The reason is due to the age and composition of the star. ...
galaxies - GEOCITIES.ws
... • After about ten billion years, a main sequence star has used up most of its hydrogen. The hydrogen core begins to contract, and the outer layers begin to expand. At that point, helium fusion begins. The star is now called a red giant. Life expectancy from here on is about one hundred million years ...
... • After about ten billion years, a main sequence star has used up most of its hydrogen. The hydrogen core begins to contract, and the outer layers begin to expand. At that point, helium fusion begins. The star is now called a red giant. Life expectancy from here on is about one hundred million years ...
How the Universe Works: Supernova Video Guide
... 4. Pressure pushes _________________ and gravity pushes _________________. 5. When energy is no longer produced in the core of the star, _________________ crushes the star. The outer layers of the star expand outwards, producing a _______________________. 6. The center of a Red Giant is crushed by _ ...
... 4. Pressure pushes _________________ and gravity pushes _________________. 5. When energy is no longer produced in the core of the star, _________________ crushes the star. The outer layers of the star expand outwards, producing a _______________________. 6. The center of a Red Giant is crushed by _ ...
Astronomy
... increase in temperature. When fusion starts to begin, that's when a protostar has been formed. If the temperature reaches about 27,000,000,000°F, nuclear fusion begins, then stars start to form. ...
... increase in temperature. When fusion starts to begin, that's when a protostar has been formed. If the temperature reaches about 27,000,000,000°F, nuclear fusion begins, then stars start to form. ...
Deep Space Mystery Note Form 2
... runs out of fuel and collapses in on itself, and ultimately the explosion leads to its death. Our Sun is not massive enough to blow itself into pieces. The Sun will expand to a red giant, turn into a planetary nebula, white dwarf and eventually end its life as a black dwarf. There are different type ...
... runs out of fuel and collapses in on itself, and ultimately the explosion leads to its death. Our Sun is not massive enough to blow itself into pieces. The Sun will expand to a red giant, turn into a planetary nebula, white dwarf and eventually end its life as a black dwarf. There are different type ...
L = σAT 4
... • The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. • The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear ...
... • The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. • The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear ...
Answer titese questions on a piece of loose leaf paper.
... I I . The Hcrczspiung-Russcll diagram shows the relationship between wliai two charaeteiistios of stars? 12- More than 90% of all stars arc cotisiderx;d stars and can be found in a diagonal path aaoss the center of the H-R diagram. 13. Within the main sequence, surface temperatures increase as absol ...
... I I . The Hcrczspiung-Russcll diagram shows the relationship between wliai two charaeteiistios of stars? 12- More than 90% of all stars arc cotisiderx;d stars and can be found in a diagonal path aaoss the center of the H-R diagram. 13. Within the main sequence, surface temperatures increase as absol ...
Lecture11
... the cloud is still in free-fall. Rotation of the cloud means this collapsing material forms a disk. Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger tha ...
... the cloud is still in free-fall. Rotation of the cloud means this collapsing material forms a disk. Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger tha ...
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.