13.5 The HR Diagram By the early 1900s, astronomers had learned
... being more luminous. Of these, the hottest are blue, and the coolest are red. Yellow stars, such as the Sun, have an intermediate temperature. Along the main sequence, a star's mass determines its position, as described by the mass–luminosity relation. Massive stars lie near the top of the main sequ ...
... being more luminous. Of these, the hottest are blue, and the coolest are red. Yellow stars, such as the Sun, have an intermediate temperature. Along the main sequence, a star's mass determines its position, as described by the mass–luminosity relation. Massive stars lie near the top of the main sequ ...
Westerlund 1 : A Super-Star Cluster within the Milky Way
... M and include NGC 3603, plus the Arches and Quintuplet clusters in the Galactic Centre. Westerlund 1 (Wd1) is a highly reddened (E(B-V)=4.5) open Galactic cluster (G339.55, -0.40) whose massive star population remains elusive. ...
... M and include NGC 3603, plus the Arches and Quintuplet clusters in the Galactic Centre. Westerlund 1 (Wd1) is a highly reddened (E(B-V)=4.5) open Galactic cluster (G339.55, -0.40) whose massive star population remains elusive. ...
1. The "Q" word and its meaning
... magnetic field, gravitational heating or other heating mechanisms, wrong treatment of the baryon density the CMB scale stops at 7 Mpc-comoving…) ...
... magnetic field, gravitational heating or other heating mechanisms, wrong treatment of the baryon density the CMB scale stops at 7 Mpc-comoving…) ...
Letter to the Editor The formation of bipolar planetary nebulae
... and one might expect that this will have an effect on the formation of the nebula. A typical post-AGB track in the HR-diagram consists of two parts (Paczyński 1971). Initially the star contracts, evolving to higher effective temperatures at a constant luminosity; then as the energy production stops ...
... and one might expect that this will have an effect on the formation of the nebula. A typical post-AGB track in the HR-diagram consists of two parts (Paczyński 1971). Initially the star contracts, evolving to higher effective temperatures at a constant luminosity; then as the energy production stops ...
The Strikingly Uniform, Highly Turbulent Interstellar Medium of the
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
Chapter 3 The Interstellar Medium
... between the stars. The mass in the gas is much larger than that in dust, with the mass of dust in the disc of our Galaxy ' 0.1 of the mass of gas. Generally, the interstellar medium amounts to only a small fraction of a galaxy’s luminous mass, but this fraction is strongly correlated with the galaxy ...
... between the stars. The mass in the gas is much larger than that in dust, with the mass of dust in the disc of our Galaxy ' 0.1 of the mass of gas. Generally, the interstellar medium amounts to only a small fraction of a galaxy’s luminous mass, but this fraction is strongly correlated with the galaxy ...
Distance to the SMC
... Since he could find no Cepheids in M31's globular clusters but many in the spiral arms, he deduced that the Cepheids in globular clusters must be Population II while the Cepheids in the spiral arms were Population I. Along with this came the realization that the globular cluster stars used by Shaple ...
... Since he could find no Cepheids in M31's globular clusters but many in the spiral arms, he deduced that the Cepheids in globular clusters must be Population II while the Cepheids in the spiral arms were Population I. Along with this came the realization that the globular cluster stars used by Shaple ...
Accretion Disk
... still be two stars: a low mass star still burning hydrogen, and a helium proto-white dwarf. The separation will be very small, and the hot core will ionize the ejected envelope, producing a planetary nebula. ...
... still be two stars: a low mass star still burning hydrogen, and a helium proto-white dwarf. The separation will be very small, and the hot core will ionize the ejected envelope, producing a planetary nebula. ...
MHD_of_Accretion_Disks
... the gas in each zone, we can calculate the emission line profile --the result is a characteristic double-horned shape ...
... the gas in each zone, we can calculate the emission line profile --the result is a characteristic double-horned shape ...
Evolution of a Planetary System
... Turn the lights off in the classroom and turn the bulb on to its highest, brightest setting. Ask the students what color the bulb is. White. Begin dimming. The color will become noticeably more yellow. Continue slowly dimming the bulb, stopping each time there is a change in color, to ask students w ...
... Turn the lights off in the classroom and turn the bulb on to its highest, brightest setting. Ask the students what color the bulb is. White. Begin dimming. The color will become noticeably more yellow. Continue slowly dimming the bulb, stopping each time there is a change in color, to ask students w ...
Dear Leif - LEIF.org
... that the interchanges considered can be realized by the fluid; one can, in principle, demonstrate stability, however, by showing that no displacement, realizable or not, can liberate energy to drive the instability. However, when the interchange is carried out in a plausible manner which avoids this ...
... that the interchanges considered can be realized by the fluid; one can, in principle, demonstrate stability, however, by showing that no displacement, realizable or not, can liberate energy to drive the instability. However, when the interchange is carried out in a plausible manner which avoids this ...
Dear Leif - LEIF.org
... that the interchanges considered can be realized by the fluid; one can, in principle, demonstrate stability, however, by showing that no displacement, realizable or not, can liberate energy to drive the instability. However, when the interchange is carried out in a plausible manner which avoids this ...
... that the interchanges considered can be realized by the fluid; one can, in principle, demonstrate stability, however, by showing that no displacement, realizable or not, can liberate energy to drive the instability. However, when the interchange is carried out in a plausible manner which avoids this ...
3.7 Isotope Effect - Institute for Astronomy | ETH
... the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the Sun and heat up. They then reradiate this heat as infrared light, in first approximation as a black-body spectrum. This radiation has to be distinguished from the v ...
... the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the Sun and heat up. They then reradiate this heat as infrared light, in first approximation as a black-body spectrum. This radiation has to be distinguished from the v ...
Space astrometry 2: Scientific results from Hipparcos
... • Ursa Major: 0.3 Gyr (Eggen 1998, Chupina et al 2001, King et al 2003) • HR 1614: 2-6 Gyr (Eggen 1998, Feltzing & Holmberg 2000) ...
... • Ursa Major: 0.3 Gyr (Eggen 1998, Chupina et al 2001, King et al 2003) • HR 1614: 2-6 Gyr (Eggen 1998, Feltzing & Holmberg 2000) ...
observing cards - NC Science Festival
... Planets orbiting new stars within open clusters likely live very chaotic lives. They have not yet formed stable orbits so collisions occur often. While our Sun was still in an open cluster, a Mars-sized planet probably slammed into Earth, eventually creating our Moon. ...
... Planets orbiting new stars within open clusters likely live very chaotic lives. They have not yet formed stable orbits so collisions occur often. While our Sun was still in an open cluster, a Mars-sized planet probably slammed into Earth, eventually creating our Moon. ...
What is a planet? - X-ray and Observational Astronomy Group
... What about the stars themselves? • Surveys began by targeting sun-like stars (spectral types F, G and K) • Now extended to M dwarfs • Incidence of planets is greatest for late F stars ...
... What about the stars themselves? • Surveys began by targeting sun-like stars (spectral types F, G and K) • Now extended to M dwarfs • Incidence of planets is greatest for late F stars ...
Lecture notes 11
... Recall that: PC ≈ G Mρ/ R and TC = ρk Therefore, as the mass increases, so does the central pressure and temperature. ...
... Recall that: PC ≈ G Mρ/ R and TC = ρk Therefore, as the mass increases, so does the central pressure and temperature. ...
Chapter three: The properties of Stars
... Chapter three: The properties of Stars When we look up into the sky in a clear night, all of the stars locate at the inner surface of a sphere called celestial sphere and they seem to be at same distance from us. However this is just a projection effect. For the stars we can see with our unaided eye ...
... Chapter three: The properties of Stars When we look up into the sky in a clear night, all of the stars locate at the inner surface of a sphere called celestial sphere and they seem to be at same distance from us. However this is just a projection effect. For the stars we can see with our unaided eye ...
Astronomy 112: The Physics of Stars Class 14 Notes: The Main
... value of 3.7 for the coefficient. This is shallower than the value of 5.6 we found for radiative stars with constant κ. As you will show on your homework, the value for radiative stars where κ is the free-free opacity differs slightly from these. II. Numerical Results on the ZAMS We have now pushed ...
... value of 3.7 for the coefficient. This is shallower than the value of 5.6 we found for radiative stars with constant κ. As you will show on your homework, the value for radiative stars where κ is the free-free opacity differs slightly from these. II. Numerical Results on the ZAMS We have now pushed ...
the magellanic clouds newsletter - Keele University Astrophysics
... have initial substructure. Furthermore, both clusters may be evolving along a very similar dynamical sequence, with the key difference that NGC 1805 is dynamically older than NGC 1818. The F-type binaries in NGC 1818 still show evidence of an initial period of rapid dynamical disruptions (which occu ...
... have initial substructure. Furthermore, both clusters may be evolving along a very similar dynamical sequence, with the key difference that NGC 1805 is dynamically older than NGC 1818. The F-type binaries in NGC 1818 still show evidence of an initial period of rapid dynamical disruptions (which occu ...
Integrated Science Names (Do with ONE partner or by yourself) How
... 5. There are an estimated 100,000,000,000 (1.0 x 1011 or 100 billion) galaxies in the universe, each with an average of 100 billion stars. Using your answer from Analysis Question #3 (how many cubic meters could hold 1 billion pellets), how large a container would you need to hold all the stars in a ...
... 5. There are an estimated 100,000,000,000 (1.0 x 1011 or 100 billion) galaxies in the universe, each with an average of 100 billion stars. Using your answer from Analysis Question #3 (how many cubic meters could hold 1 billion pellets), how large a container would you need to hold all the stars in a ...
