Powerpoint - Physics and Astronomy
... As stars evolve during their main-sequence lifetime a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteristics of surfa ...
... As stars evolve during their main-sequence lifetime a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteristics of surfa ...
Question 1 The star Regulus, in the constellation Leo, appears
... . Which statement best describes the “fabric” of space and time as outlined by the classical physics of Newton? ...
... . Which statement best describes the “fabric” of space and time as outlined by the classical physics of Newton? ...
Folie 1
... Evolution to Red Giant • Once the star uses up all the H in its convective core, nuclear fusion ceases, convection is quenched. The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the ...
... Evolution to Red Giant • Once the star uses up all the H in its convective core, nuclear fusion ceases, convection is quenched. The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the ...
CS3_Ch 3 - Leon County Schools
... • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. ...
... • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. ...
Bright versus Nearby Stars
... represented in the bright stars. • Over 1/3 of the bright stars are O & B types. • Only 13% are solar-type G stars. • 26% of the bright stars are K & M type. ...
... represented in the bright stars. • Over 1/3 of the bright stars are O & B types. • Only 13% are solar-type G stars. • 26% of the bright stars are K & M type. ...
Rotation in the ZAMS: Be and Bn stars
... Figure 3a shows the apparent V=7 magnitude limited counts of dwarf Be stars relative to dwarf B stars. There is an apparent lack of dwarf Be stars cooler than spectral type B7. This could be due to genuine Be stars whose discs are minute and/or too cool for the Hα emission be detectable and/or, to f ...
... Figure 3a shows the apparent V=7 magnitude limited counts of dwarf Be stars relative to dwarf B stars. There is an apparent lack of dwarf Be stars cooler than spectral type B7. This could be due to genuine Be stars whose discs are minute and/or too cool for the Hα emission be detectable and/or, to f ...
talk / PPT / 1.6 MB
... Milky Way compared to External discs Where does the Milky Way lie on the ...
... Milky Way compared to External discs Where does the Milky Way lie on the ...
Welcome to Astro 10! - UC Berkeley Astronomy w
... A Sense of Scale • What if the Sun (1.4 x 106 km diameter) was shrunken to the size of a period (0.5 mm)? • The nearest star would be 14 km (9 miles) away! (The distance to San Francisco!) • The size of the Milky Way Galaxy would be about 320,000 km, almost the distance to the Moon! • The nearest g ...
... A Sense of Scale • What if the Sun (1.4 x 106 km diameter) was shrunken to the size of a period (0.5 mm)? • The nearest star would be 14 km (9 miles) away! (The distance to San Francisco!) • The size of the Milky Way Galaxy would be about 320,000 km, almost the distance to the Moon! • The nearest g ...
12 Introduction to Cepheid Variable Stars Exercise
... If you know the distance to the bulb and measure its apparent brightness then you can calculate the wattage of the bulb. Likewise, if you know the wattage of the bulb and measure the observed brightness you can calculate the distance to the bulb. This can be applied to stars, if you determine the ap ...
... If you know the distance to the bulb and measure its apparent brightness then you can calculate the wattage of the bulb. Likewise, if you know the wattage of the bulb and measure the observed brightness you can calculate the distance to the bulb. This can be applied to stars, if you determine the ap ...
Geller Slides on Contact with ET
... – Right environmental conditions • Especially for liquid water ...
... – Right environmental conditions • Especially for liquid water ...
The Life Cycle of A Star
... inside a black hole. Nevertheless, there is now a great deal of observational evidence for the existence of two types of black holes: those with masses of a typical star (4-15 times the mass of our Sun), and those with masses of a typical galaxy. This evidence comes not from seeing the black holes d ...
... inside a black hole. Nevertheless, there is now a great deal of observational evidence for the existence of two types of black holes: those with masses of a typical star (4-15 times the mass of our Sun), and those with masses of a typical galaxy. This evidence comes not from seeing the black holes d ...
Black Hole
... •There are many galaxies in the universe, and our Another galaxy , The galaxy, the Milky Way Canis Major Dwarf, was found by German galaxy, has many solar Astronomers on November systems and planets in it. 10, 2010. This is currently the closest galaxy to our ...
... •There are many galaxies in the universe, and our Another galaxy , The galaxy, the Milky Way Canis Major Dwarf, was found by German galaxy, has many solar Astronomers on November systems and planets in it. 10, 2010. This is currently the closest galaxy to our ...
Slide 1
... understand how clumping changes as a function of radial distance, thus providing reliable mass loss rates, (ii) study for the first time how clumping changes as a function of temperature, luminosity and rotation in supergiants, giants and main-sequence stars. The high quality imaging capabilities of ...
... understand how clumping changes as a function of radial distance, thus providing reliable mass loss rates, (ii) study for the first time how clumping changes as a function of temperature, luminosity and rotation in supergiants, giants and main-sequence stars. The high quality imaging capabilities of ...
Powerpoint of lecture 14
... • Post-MS timescale also nuclear (except for a few phases) – so again much more data than for pre-MS studies • Two kinds of observational constraint Statistical studies of large numbers of field stars (problem: selection effects, e.g. more luminous stars dominate sample) Look at star clusters: s ...
... • Post-MS timescale also nuclear (except for a few phases) – so again much more data than for pre-MS studies • Two kinds of observational constraint Statistical studies of large numbers of field stars (problem: selection effects, e.g. more luminous stars dominate sample) Look at star clusters: s ...
December 2015 - Hermanus Astronomy
... “We will use Curiosity to learn whether the wind is actually sorting the minerals in the dunes by how the wind transports particles of different grain size,” said Bethany Ehlmann of the California Institute of Technology and NASA’s Jet Propulsion Laboratory, both in Pasadena, California. As an examp ...
... “We will use Curiosity to learn whether the wind is actually sorting the minerals in the dunes by how the wind transports particles of different grain size,” said Bethany Ehlmann of the California Institute of Technology and NASA’s Jet Propulsion Laboratory, both in Pasadena, California. As an examp ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.