Unit 1
... • A. They are grouped into clusters that in turn are grouped into clusters of clusters (superclusters) • B. Galaxies are spread more or less evenly throughout the Universe • C. They are grouped around our galaxy • D. none of the above ...
... • A. They are grouped into clusters that in turn are grouped into clusters of clusters (superclusters) • B. Galaxies are spread more or less evenly throughout the Universe • C. They are grouped around our galaxy • D. none of the above ...
Stars, Galaxies, and the Universe Section 1 Section 1
... stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less massive. ...
... stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less massive. ...
Support worksheet – Topic 3 Questions
... Suggest why the stellar parallax method is limited to distances of about 300 pc for Earth-based telescopes but can be extended to 1000 pc for satellite-based telescopes. ...
... Suggest why the stellar parallax method is limited to distances of about 300 pc for Earth-based telescopes but can be extended to 1000 pc for satellite-based telescopes. ...
Seasons and the Changing Sky
... • Find the two stars that make up the end of the “bowl” in the Big Dipper • An imaginary line drawn between the two will lead you right to Polaris! ...
... • Find the two stars that make up the end of the “bowl” in the Big Dipper • An imaginary line drawn between the two will lead you right to Polaris! ...
Chapter 28 Stars and Galaxies Reading Guide
... magnitude of –26.7. How could this be true? The friend can be referring to absolute magnitude and not apparent magnitude ...
... magnitude of –26.7. How could this be true? The friend can be referring to absolute magnitude and not apparent magnitude ...
17 The Deaths of Stars
... The expansion velocities of the material in the Crab Nebula, measured using Doppler shifts, and its size can be used to calculate the time of the original explosion which agrees within experimental error to the observed explosion in 1054 CE. There is a neutron star (pulsar) at the center of the Crab ...
... The expansion velocities of the material in the Crab Nebula, measured using Doppler shifts, and its size can be used to calculate the time of the original explosion which agrees within experimental error to the observed explosion in 1054 CE. There is a neutron star (pulsar) at the center of the Crab ...
Astronomy In the News Parallax Class demos: Parallax
... a) 2 pc = 6.5 light years b) 20 pc = 65 light years c) 200 pc = 650 light years ...
... a) 2 pc = 6.5 light years b) 20 pc = 65 light years c) 200 pc = 650 light years ...
Lecture Eight (Powerpoint format) - Flash
... The collapse of the disk is arrested at the center once the gas begins to heat up and can support itself under its own weight. At this point, the central “core” is entirely molecular in composition, is a few hundreds of degrees at its surface, and has a radius of a few AU (comparable to the orbi ...
... The collapse of the disk is arrested at the center once the gas begins to heat up and can support itself under its own weight. At this point, the central “core” is entirely molecular in composition, is a few hundreds of degrees at its surface, and has a radius of a few AU (comparable to the orbi ...
Outline2a
... As the gas cloud collapses, the protostar gets smaller and smaller (and, due to the increased central pressure), hotter and hotter. Accretion will cause the mass of the protostar to increase more than 100 times. The star will move towards its place on the ...
... As the gas cloud collapses, the protostar gets smaller and smaller (and, due to the increased central pressure), hotter and hotter. Accretion will cause the mass of the protostar to increase more than 100 times. The star will move towards its place on the ...
Chapter 2 Basic Chemistry
... pure energy. There was a period of rapid expansion that caused the energy to cool and allowed sub-atomic particles, such as protons, electrons, and neutrons, to form. Hydrogen nuclei began forming about one second after the big bang, but the temperature was still too high for atoms to form and remai ...
... pure energy. There was a period of rapid expansion that caused the energy to cool and allowed sub-atomic particles, such as protons, electrons, and neutrons, to form. Hydrogen nuclei began forming about one second after the big bang, but the temperature was still too high for atoms to form and remai ...
Question C:
... Zeilik, Fig. 13-10 is an HR (color-magnitude) diagram for the globular cluster M3. At B-V=0.4, where there are some obvious main sequence stars, we read 18.5 ≤ mV ≤ 19.5 We can find the absolute magnitude MV at B-4=0.4 from a couple of places: • Table A4-3 says that MV≈3.5 • The HR diagram used with ...
... Zeilik, Fig. 13-10 is an HR (color-magnitude) diagram for the globular cluster M3. At B-V=0.4, where there are some obvious main sequence stars, we read 18.5 ≤ mV ≤ 19.5 We can find the absolute magnitude MV at B-4=0.4 from a couple of places: • Table A4-3 says that MV≈3.5 • The HR diagram used with ...
Characteristics of Main Sequence Stars
... nuclear reactions in high mass stars are generally confined to a very small region, much smaller than the size of the convective core. • As the stellar mass increases, so does the size of the convective core (due again to the large increase in ² with temperature). Supermassive stars with M ∼ 100M¯ w ...
... nuclear reactions in high mass stars are generally confined to a very small region, much smaller than the size of the convective core. • As the stellar mass increases, so does the size of the convective core (due again to the large increase in ² with temperature). Supermassive stars with M ∼ 100M¯ w ...
Oscillating White Dwarf Stars Background on White Dwarfs
... • In 1979 McGraw and collaborators discovered pulsations in the WD PG 1159-035 that showed multi-periodic variations like in ZZ Ceti stars, but it was much hotter T~150000 K • Post Asymptotic giant branch (AGB). A violent mixing event is induced by a helium flash in the post-AGB phase produces an en ...
... • In 1979 McGraw and collaborators discovered pulsations in the WD PG 1159-035 that showed multi-periodic variations like in ZZ Ceti stars, but it was much hotter T~150000 K • Post Asymptotic giant branch (AGB). A violent mixing event is induced by a helium flash in the post-AGB phase produces an en ...
The Properties of Stars
... Finding the Masses of Spectroscopic Binaries Finding the mass of the stars in a binary star system requires observations that give (a) the sum of the masses and (b) the ratio of the masses. This can easily be done if the system is a well-observed visual binary. In that case, we can plot the orbit a ...
... Finding the Masses of Spectroscopic Binaries Finding the mass of the stars in a binary star system requires observations that give (a) the sum of the masses and (b) the ratio of the masses. This can easily be done if the system is a well-observed visual binary. In that case, we can plot the orbit a ...
here - British Astronomical Association
... like a balloon blowing up and down – only outer layers involved. • Periods range from hours to years, depending type. ...
... like a balloon blowing up and down – only outer layers involved. • Periods range from hours to years, depending type. ...
Spying into the lives of the stars
... To introduce the lab, ask students what they know about stars. Explaint that we know that, like humans, stars are born, grow up, and die. It’s just that stars take longer to do these things: millions and billions of years. You can’t really just take a single star and follow it from birth to death, s ...
... To introduce the lab, ask students what they know about stars. Explaint that we know that, like humans, stars are born, grow up, and die. It’s just that stars take longer to do these things: millions and billions of years. You can’t really just take a single star and follow it from birth to death, s ...
Teachers Notes - Edinburgh International Science Festival
... Our solar system’s structure has a star (our sun) at the centre with planets, dwarf planets, asteroids, comets and satellites all moving in approximately circular paths around it. This movement is known as orbiting. These objects stay in orbit due to the gravitational force between them and the sun. ...
... Our solar system’s structure has a star (our sun) at the centre with planets, dwarf planets, asteroids, comets and satellites all moving in approximately circular paths around it. This movement is known as orbiting. These objects stay in orbit due to the gravitational force between them and the sun. ...
Apparent Magnitude
... extremely luminous object. The explosion expels much or all of a star's material at a velocity of up to a tenth the speed of light, driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. ...
... extremely luminous object. The explosion expels much or all of a star's material at a velocity of up to a tenth the speed of light, driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. ...
Luminosity - UCF Physics
... measure its distance and apparent brightness: Luminosity = 4π (distance)2 x (Brightness) Note that there is a huge range in stellar ...
... measure its distance and apparent brightness: Luminosity = 4π (distance)2 x (Brightness) Note that there is a huge range in stellar ...
The Life of a Star - Department of Physics and Astronomy
... Young star clusters give insight into star formation and evolution • Newborn stars may form an open or galactic cluster • Stars are held together in such a cluster by gravity • Occasionally a star moving more rapidly than average will escape, or leave the cluster • A stellar association is a group ...
... Young star clusters give insight into star formation and evolution • Newborn stars may form an open or galactic cluster • Stars are held together in such a cluster by gravity • Occasionally a star moving more rapidly than average will escape, or leave the cluster • A stellar association is a group ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.