Shining Light on the Stars: The Hertzsprung-Russell
... most of which are too faint to be seen without a telescope? We immediately see that these two groups of stars lie in completely different parts of the HR diagram. The local group of stars within 25 light years of the Sun are cooler and less luminous than the Sun, while the stars we can see in the ni ...
... most of which are too faint to be seen without a telescope? We immediately see that these two groups of stars lie in completely different parts of the HR diagram. The local group of stars within 25 light years of the Sun are cooler and less luminous than the Sun, while the stars we can see in the ni ...
Star Life Cycle
... The more massive stars the heavier the star the heavier the elements. Which is where most of the heavy elements in the universe are made. Throughout this whole process is that battle between gravity and gas pressure, known as ...
... The more massive stars the heavier the star the heavier the elements. Which is where most of the heavy elements in the universe are made. Throughout this whole process is that battle between gravity and gas pressure, known as ...
Galaxy Formation and Evolution Open Problems
... • moderately old stars with low specific angular momentum. • Wide range of metallicity • Triaxial shape (central bar) • Central supermassive BH Stellar Halo • 109 old and metal poor stars (Pop.II) • 150 globular clusters (13 Gyr) • <0.2% Galaxy mass, 2% of the light •Dark Halo ...
... • moderately old stars with low specific angular momentum. • Wide range of metallicity • Triaxial shape (central bar) • Central supermassive BH Stellar Halo • 109 old and metal poor stars (Pop.II) • 150 globular clusters (13 Gyr) • <0.2% Galaxy mass, 2% of the light •Dark Halo ...
ASTR-1020: Astronomy II Course Lecture Notes Section III
... 3. M stars have a large amount of molecular absorption features called molecular bands. TiO is very strong in the visible portion of the spectrum. a) C stars (a special class of cool stars) have a higher abundance of carbon (C/O > 1) with respect to the M stars (which have C/O < 1) =⇒ strong C2 and ...
... 3. M stars have a large amount of molecular absorption features called molecular bands. TiO is very strong in the visible portion of the spectrum. a) C stars (a special class of cool stars) have a higher abundance of carbon (C/O > 1) with respect to the M stars (which have C/O < 1) =⇒ strong C2 and ...
review_one - MSU Solar Physics
... Go to the following rooms, based on team number: Teams 1-33: EPS 103 Teams 34-66: Leon Johnson 339 Teams 67-100: Roberts 101 Understand and be prepared to explain the following: Unit 1 The three components to measuring radiation The difference between light gathering power and resolving power ...
... Go to the following rooms, based on team number: Teams 1-33: EPS 103 Teams 34-66: Leon Johnson 339 Teams 67-100: Roberts 101 Understand and be prepared to explain the following: Unit 1 The three components to measuring radiation The difference between light gathering power and resolving power ...
SHELL H II REGIONS IN NGC 6334
... • However, A1 has been proposed in the past to be shock with ambient medium ...
... • However, A1 has been proposed in the past to be shock with ambient medium ...
Centimeter and Millimeter Observations of Very Young Binary Systems
... • However, A1 has been proposed in the past to be shock with ambient medium ...
... • However, A1 has been proposed in the past to be shock with ambient medium ...
Untitled
... One light year is the distance light travels in one year 1 light year ~ 60,000 AU 1 light year ~ 1013 km Distance to Sun is ~ 8 light-minutes ...
... One light year is the distance light travels in one year 1 light year ~ 60,000 AU 1 light year ~ 1013 km Distance to Sun is ~ 8 light-minutes ...
AST301.Ch22.NeutGammBH - University of Texas Astronomy
... First indication: they are distributed isotropically in the sky (no preferred direction, like the plane of the Milky Way if they were in our Galactic disk). But they could be in the Oort comet cloud surrounding our solar system, or in the halo of our Galaxy, or… Then in 1997 it was possible (from th ...
... First indication: they are distributed isotropically in the sky (no preferred direction, like the plane of the Milky Way if they were in our Galactic disk). But they could be in the Oort comet cloud surrounding our solar system, or in the halo of our Galaxy, or… Then in 1997 it was possible (from th ...
First young loose association in the northern hemisphere?
... intermediate- and high-resolution spectroscopic observations of this sample allowed us to discover additional lithium-rich sources. Our preliminary results show that some of them share the same space motion as our 4 original stars. They have properties rather similar to the members of the TW Hydrae ...
... intermediate- and high-resolution spectroscopic observations of this sample allowed us to discover additional lithium-rich sources. Our preliminary results show that some of them share the same space motion as our 4 original stars. They have properties rather similar to the members of the TW Hydrae ...
1. Stellar Evolution – Notes Astronomers classify stars according to
... the normal convention, where values increase going left to right on an axis. The temperature may be replaced or supplemented with spectral class. The luminosity scale on the left axis is dimmest on the bottom and gets brighter towards the top. This places the cooler, dimmer stars towards the lower r ...
... the normal convention, where values increase going left to right on an axis. The temperature may be replaced or supplemented with spectral class. The luminosity scale on the left axis is dimmest on the bottom and gets brighter towards the top. This places the cooler, dimmer stars towards the lower r ...
Star Formation
... protostar looks starlike after the surrounding gas is blown away, but its thermal energy comes from gravitational contraction, not fusion 4) The collapsing gas becomes a young stellar object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it become ...
... protostar looks starlike after the surrounding gas is blown away, but its thermal energy comes from gravitational contraction, not fusion 4) The collapsing gas becomes a young stellar object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it become ...
Measuring large distances
... So based on the color of a star, and how bright it is, it’s possible to make a guess about how far away the star is. ...
... So based on the color of a star, and how bright it is, it’s possible to make a guess about how far away the star is. ...
129 DYNAMICAL STREAMS IN THE SOLAR NEIGHBOURHOOD B
... which partly evaporated with time, those kinematically cold groups are generally called superclusters (namely the Hyades and Sirius superclusters). They are also often called streams or moving groups. During the last fifteen years, Eggen’s hypothesis that these groups are in fact cluster remnants ha ...
... which partly evaporated with time, those kinematically cold groups are generally called superclusters (namely the Hyades and Sirius superclusters). They are also often called streams or moving groups. During the last fifteen years, Eggen’s hypothesis that these groups are in fact cluster remnants ha ...
Diapositiva 1
... nebulae have long been appreciated as a final phase in the life of a sunlike star. Only much more recently however, have some planetaries been found to have halos like this one, likely formed of material shrugged off during earlier active episodes in the star's evolution. While the planetary nebula ...
... nebulae have long been appreciated as a final phase in the life of a sunlike star. Only much more recently however, have some planetaries been found to have halos like this one, likely formed of material shrugged off during earlier active episodes in the star's evolution. While the planetary nebula ...
Linking Asteroids and Meteorites through Reflectance
... • Gravity shrinks the inert helium core and surrounding shell of hydrogen • The shell of hydrogen becomes hot for fusion • This is called hydrogen-shell burning ...
... • Gravity shrinks the inert helium core and surrounding shell of hydrogen • The shell of hydrogen becomes hot for fusion • This is called hydrogen-shell burning ...
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.