Chemical abundances and winds of massive stars in M31: a B
... stellar wind properties of O-, B- and A-supergiants in Local Group galaxies with well defined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identified OB and WR stars beyond the Magellanic Clouds e.g. Masse ...
... stellar wind properties of O-, B- and A-supergiants in Local Group galaxies with well defined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identified OB and WR stars beyond the Magellanic Clouds e.g. Masse ...
2. The Anatomy of Stellar Life and Death
... and Peter Schilke (University of Cologne) of a star-forming region IRAS 19410–2336 revealed that the process of massive stars formation appeared to mirror that of lower mass star formation with a very similar scaling of the mass of protostars. The observations were done in the millimeter (microwave) ...
... and Peter Schilke (University of Cologne) of a star-forming region IRAS 19410–2336 revealed that the process of massive stars formation appeared to mirror that of lower mass star formation with a very similar scaling of the mass of protostars. The observations were done in the millimeter (microwave) ...
Project 8 : Stellar Spectra: Classification
... Absorption lines occur when an electron absorbs energy from the spectrum to move up the energy levels in the atom. Since hydrogen has only one electron, this electron is usually in the ground state. But as the temperature rises, the average electron gains m ...
... Absorption lines occur when an electron absorbs energy from the spectrum to move up the energy levels in the atom. Since hydrogen has only one electron, this electron is usually in the ground state. But as the temperature rises, the average electron gains m ...
12C13C1414N21312C/13C3he43He/4He Sub-surface
... While the envelope convection zones may, at first glance, be negligible for the internal evolution of hot massive stars, they may cause observable phenomena at the stellar surface. The reason is that the zones are located very close to the photosphere for some mass interval (see below). Here, we wil ...
... While the envelope convection zones may, at first glance, be negligible for the internal evolution of hot massive stars, they may cause observable phenomena at the stellar surface. The reason is that the zones are located very close to the photosphere for some mass interval (see below). Here, we wil ...
Altair - the hottest `cool` star in X-rays
... 2.4 MK and its emission measure distribution (EMD) is dominated by rather cool plasma at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quie ...
... 2.4 MK and its emission measure distribution (EMD) is dominated by rather cool plasma at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quie ...
Introduction - Cambridge University Press
... structure and behaviour of stars. We review the Hertzsprung–Russell diagram, introduce some parameters of the Sun as a typical star, and consider the general equations of stellar structure. We then present a summary of the nuclear fusion reactions that occur in main-sequence stars and consider the a ...
... structure and behaviour of stars. We review the Hertzsprung–Russell diagram, introduce some parameters of the Sun as a typical star, and consider the general equations of stellar structure. We then present a summary of the nuclear fusion reactions that occur in main-sequence stars and consider the a ...
the link to the powerpoint for Monday
... intrinsic POWER of object shining light. • Total of all emitted/radiated energy every second. • Intrinsic • What does intrinsic mean? ...
... intrinsic POWER of object shining light. • Total of all emitted/radiated energy every second. • Intrinsic • What does intrinsic mean? ...
Neil F. Comins - Kuwait Life Sciences Company
... PREFACE away. View 2,500,000 stars along with more than 170 deep-space objects such as galaxies, star clusters, and nebulae. Travel 15,000 years in time, check out the view from the International Space Station, and see planets up close from any one of their moons. Included are stunning OpenGL graph ...
... PREFACE away. View 2,500,000 stars along with more than 170 deep-space objects such as galaxies, star clusters, and nebulae. Travel 15,000 years in time, check out the view from the International Space Station, and see planets up close from any one of their moons. Included are stunning OpenGL graph ...
The Milky Way: Spiral galaxies:
... •! Spirals show HI disks (amount of HI depends on Hubble type) •! HI gas is optically thin: the 21 cm line suffers almost no absorption. Note that spin flips are classically “forbidden”: on average, a single hydrogen atom will take 107 years to decay! The probability of an absorption is even rarer. ...
... •! Spirals show HI disks (amount of HI depends on Hubble type) •! HI gas is optically thin: the 21 cm line suffers almost no absorption. Note that spin flips are classically “forbidden”: on average, a single hydrogen atom will take 107 years to decay! The probability of an absorption is even rarer. ...
Solar-type dynamo behaviour in fully convective stars without a
... to X-ray wavelengths. The dynamo responsible for generating the field depends on the shearing of internal magnetic fields by differential rotation1,2. The shearing has long been thought to take place in a boundary layer known as the tachocline between the radiative core and the convective envelope3. ...
... to X-ray wavelengths. The dynamo responsible for generating the field depends on the shearing of internal magnetic fields by differential rotation1,2. The shearing has long been thought to take place in a boundary layer known as the tachocline between the radiative core and the convective envelope3. ...
VISIBLE STARS AS APPARENT OBSERVATIONAL EVIDENCE IN
... stars are defined, spherical, consistently measurable celestial bodies that are suns scattered throughout space. ...
... stars are defined, spherical, consistently measurable celestial bodies that are suns scattered throughout space. ...
Station A Star Charts I
... D6. (2 pts) When modern astronomers redesigned the magnitude system, they set the scale so that every five magnitudes is 100 times brighter (or dimmer, depending on direction). If star A is 1 magnitude brighter than star B, how many times brighter is it? Give your answer to the nearest thousandth. ...
... D6. (2 pts) When modern astronomers redesigned the magnitude system, they set the scale so that every five magnitudes is 100 times brighter (or dimmer, depending on direction). If star A is 1 magnitude brighter than star B, how many times brighter is it? Give your answer to the nearest thousandth. ...
5 Report of the Panel on Stars and Stellar Evolution
... cosmic expansion; but because this understanding is not complete, there is much to learn about the subtle interplay of convection, rotation, and magnetism or the not-so-subtle violent events that destroy stars or transform them into neutron stars or black holes. Although the topics of stars and thei ...
... cosmic expansion; but because this understanding is not complete, there is much to learn about the subtle interplay of convection, rotation, and magnetism or the not-so-subtle violent events that destroy stars or transform them into neutron stars or black holes. Although the topics of stars and thei ...
Between the Stars: Gas and Dust in Space
... To understand how stars form, we need to know the raw material from which they are made All the gas and dust material that lies in the region between stars is referred to as interstellar matter The entire collection of interstellar matter is called the interstellar medium The interstellar medium acc ...
... To understand how stars form, we need to know the raw material from which they are made All the gas and dust material that lies in the region between stars is referred to as interstellar matter The entire collection of interstellar matter is called the interstellar medium The interstellar medium acc ...
The self-enrichment of galactic halo globular clusters: a clue to their
... observations. De Marchi et al. (1999) have observed the globular cluster NGC 6712 with the ESO-VLT and derived its mass function. Contrary to other globular clusters, NGC 6712 mass function shows a noticeable deficit in stars with masses below 0.75M⊙. Since this object, in its galactic orbit, has re ...
... observations. De Marchi et al. (1999) have observed the globular cluster NGC 6712 with the ESO-VLT and derived its mass function. Contrary to other globular clusters, NGC 6712 mass function shows a noticeable deficit in stars with masses below 0.75M⊙. Since this object, in its galactic orbit, has re ...
Life as a Low Mass Red Giant
... just leaving the Main Sequence is called "main sequence turnoff" point. http://www.astro.ubc.ca/~scharein/a311/Sim.html The age of a cluster is just the main sequence lifetime of the stars at the main sequence turnoff • This is about the only way astronomers have to estimate the age of objects outsi ...
... just leaving the Main Sequence is called "main sequence turnoff" point. http://www.astro.ubc.ca/~scharein/a311/Sim.html The age of a cluster is just the main sequence lifetime of the stars at the main sequence turnoff • This is about the only way astronomers have to estimate the age of objects outsi ...
Why Study Cosmic Near Infrared Background? (1-4um)
... background cannot originate from high-z galaxies, because such galaxies are not seen in high-z galaxy surveys. ...
... background cannot originate from high-z galaxies, because such galaxies are not seen in high-z galaxy surveys. ...
Chapter 11
... 11.5 Stars of Other Masses This H–R diagram shows the evolution of stars somewhat more and somewhat less massive than the Sun. The shape of the paths is similar, but they wind up in different places on the main sequence. ...
... 11.5 Stars of Other Masses This H–R diagram shows the evolution of stars somewhat more and somewhat less massive than the Sun. The shape of the paths is similar, but they wind up in different places on the main sequence. ...
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.