Lifecycle of Stars
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a personal poster that visually displays the four life cycles. You will work in table teams to complete this process, but you will each create your own mini-poster. 2) Use your n ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a personal poster that visually displays the four life cycles. You will work in table teams to complete this process, but you will each create your own mini-poster. 2) Use your n ...
Stellar Evolution
... it creates a stronger gravitational field and heats up. Making “protostars” ...
... it creates a stronger gravitational field and heats up. Making “protostars” ...
Foundation 1 - Discovering Astronomy
... core continues to contract and eventually becomes hot enough (100 million kelvins) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy – occurs rapidly - called the Helium Flash ...
... core continues to contract and eventually becomes hot enough (100 million kelvins) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy – occurs rapidly - called the Helium Flash ...
Life Cycle of a Star
... The color of a star is dependant on its temperature. Astronomers measure the temperature of each star by its outer most layer or its photosphere. O stars, which are the hottest of the seven categories, are blue in color. M stars, which are the coolest, are red. Within the range of this spectrum, the ...
... The color of a star is dependant on its temperature. Astronomers measure the temperature of each star by its outer most layer or its photosphere. O stars, which are the hottest of the seven categories, are blue in color. M stars, which are the coolest, are red. Within the range of this spectrum, the ...
Our Community`s Place Among the Stars
... upper left to the lower right of the H-R diagram Many stars spend 90% of their lifetime on the main sequence Our sun ...
... upper left to the lower right of the H-R diagram Many stars spend 90% of their lifetime on the main sequence Our sun ...
Module G - U1_ L3 - Life Cycle of Stars
... • As a result, dense regions of gas and dust form within the nebula. • The densest regions, called dense cores, form new stars. • The temperature within dense cores increases for millions of years. • At about 10 million °C, the process of hydrogen nuclear fusion begins, marking the birth of a star. ...
... • As a result, dense regions of gas and dust form within the nebula. • The densest regions, called dense cores, form new stars. • The temperature within dense cores increases for millions of years. • At about 10 million °C, the process of hydrogen nuclear fusion begins, marking the birth of a star. ...
Aging nearby spiral galaxies using H
... IMF: total number of stars of a certain mass range initially created per unit volume » “Determines the evolution, surface brightness, chemical ...
... IMF: total number of stars of a certain mass range initially created per unit volume » “Determines the evolution, surface brightness, chemical ...
Star Formation
... and spend most of their lives • Once on the main sequence, a star stays in the same location on the H-R diagram until it runs out of fuel and begins to die ...
... and spend most of their lives • Once on the main sequence, a star stays in the same location on the H-R diagram until it runs out of fuel and begins to die ...
Methods of Energy Transport There are 3 methods for energy
... To decide whether convection occurs in a star, begin by considering a blob of material with volume V in pressure equilibrium with its surroundings. Initially, both the blob and its surroundings have temperature T1 and density ρ1 . Now suppose the blob’s temperature is perturbed, such that its new te ...
... To decide whether convection occurs in a star, begin by considering a blob of material with volume V in pressure equilibrium with its surroundings. Initially, both the blob and its surroundings have temperature T1 and density ρ1 . Now suppose the blob’s temperature is perturbed, such that its new te ...
Spectral Classification and the HR Diagram
... As director of the Harvard College Observatory Edward C. Pickering (1846-1919) undertook the oversight for completion of the Henry Draper Catalogue. Because it was the goal of this project to classify a sufficient number of stars so that it would be years before anyone felt the need to repeat such a ...
... As director of the Harvard College Observatory Edward C. Pickering (1846-1919) undertook the oversight for completion of the Henry Draper Catalogue. Because it was the goal of this project to classify a sufficient number of stars so that it would be years before anyone felt the need to repeat such a ...
Classifying Stars - Concord Academy Boyne
... What is Stellar Classification? The classification of stars is based on the elements they absorb and their temperature, and are listed from hottest to coldest ...
... What is Stellar Classification? The classification of stars is based on the elements they absorb and their temperature, and are listed from hottest to coldest ...
ASTR 1120H – Spring Semester 2010 Exam 2 – Answers The
... attraction causes a clump of material to condense into a protostar. Subsequent contraction causes the protostar to heat up and begin glowing. When its core temperature becomes high enough, it begins thermonuclear fusion, at which point it's a full-fledged star and is situated on the main sequence of ...
... attraction causes a clump of material to condense into a protostar. Subsequent contraction causes the protostar to heat up and begin glowing. When its core temperature becomes high enough, it begins thermonuclear fusion, at which point it's a full-fledged star and is situated on the main sequence of ...
Star Formation
... • The time required for an interstellar cloud to become a main sequence star depends strongly on its mass • The most massive O stars reach the 10 million Kelvin needed to start fusion in a million years (1/50 time ...
... • The time required for an interstellar cloud to become a main sequence star depends strongly on its mass • The most massive O stars reach the 10 million Kelvin needed to start fusion in a million years (1/50 time ...
Section 3-3(rev04) 2
... depending on how large they are. • When fuel runs out, it becomes a white dwarf, neutron star, or black hole. • Small and medium stars become red giants and then white dwarfs. These are the size of the Earth but have the mass of the sun, so it is very dense. A spoonful of white dwarf is equal to a t ...
... depending on how large they are. • When fuel runs out, it becomes a white dwarf, neutron star, or black hole. • Small and medium stars become red giants and then white dwarfs. These are the size of the Earth but have the mass of the sun, so it is very dense. A spoonful of white dwarf is equal to a t ...
Lab 5 Takehome
... Figure 2 shows the same stars, but here what’s plotted is the apparent brightness of the star as seen from the Earth, instead of the luminosity. The vertical axis is scaled so that 1.0 represe ...
... Figure 2 shows the same stars, but here what’s plotted is the apparent brightness of the star as seen from the Earth, instead of the luminosity. The vertical axis is scaled so that 1.0 represe ...
solutions
... Recall that a photon produced by fusion in the Sun’s core does not pass through the star directly but interacts with the remainder of the Sun’s mass on the way out. The random-walk process, radiative diffusion, causes the photon to take millions years to reach the surface of the Sun. So if fusion in ...
... Recall that a photon produced by fusion in the Sun’s core does not pass through the star directly but interacts with the remainder of the Sun’s mass on the way out. The random-walk process, radiative diffusion, causes the photon to take millions years to reach the surface of the Sun. So if fusion in ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
1 Star Formation and Main Sequence Evolution Condensation
... up they move on the H-R diagram towards the main sequence Mass loss can only occur perpendicular to the protoplanetary disc leading to the formation of a bipolar outflow ...
... up they move on the H-R diagram towards the main sequence Mass loss can only occur perpendicular to the protoplanetary disc leading to the formation of a bipolar outflow ...
Slide 1 - Beverley High School
... • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
... • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
ISP 205 Review Questions, Week 10
... Why don’t all of the pieces just pull themselves together into an infinitesimally small clump at the center? ...
... Why don’t all of the pieces just pull themselves together into an infinitesimally small clump at the center? ...