Slide 1
... Comprised of 2 stars in a close orbit around each other (i.e., a binary system). They are tidally locked (i.e., rotation period equals orbital period, of only days). ...
... Comprised of 2 stars in a close orbit around each other (i.e., a binary system). They are tidally locked (i.e., rotation period equals orbital period, of only days). ...
The Evolution of Stars - a More Detailed Picture (Chapter 8
... As the star expands, however, the effective temperature cannot continue to fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces ...
... As the star expands, however, the effective temperature cannot continue to fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces ...
vuorinen_neutron_stars
... 2. but not impossible if you systematically use 1st principles results at low and high density 3. Discovering massive stars places strong constraints on nuclear matter EoS due to tension with soft pQCD pressure 4. pQCD constraint useful even if no quark matter present in stars ...
... 2. but not impossible if you systematically use 1st principles results at low and high density 3. Discovering massive stars places strong constraints on nuclear matter EoS due to tension with soft pQCD pressure 4. pQCD constraint useful even if no quark matter present in stars ...
Make Your Own Star Bracelet
... layers of gas, leaving a small core that shines out radio waves as the stars rotate very fast. Astronomers did no know about these stars until they became using radio telescopes in the 1960s. Because they appear to pulse out radio waves as they spin, the are sometimes called pulsars. (pick up the bl ...
... layers of gas, leaving a small core that shines out radio waves as the stars rotate very fast. Astronomers did no know about these stars until they became using radio telescopes in the 1960s. Because they appear to pulse out radio waves as they spin, the are sometimes called pulsars. (pick up the bl ...
1. Basic Properties of Stars
... no absorption of photons. At low densities, collisions between atoms are rare and they are not ionized. At higher densities, more and more of the atoms of a particular element become ionized, and the spectral lines become weak. One way to increase density at the surface of a star is by increasing su ...
... no absorption of photons. At low densities, collisions between atoms are rare and they are not ionized. At higher densities, more and more of the atoms of a particular element become ionized, and the spectral lines become weak. One way to increase density at the surface of a star is by increasing su ...
pptx
... because carbon nuclei have an energy level at exactly the right place otherwise carbon would be a rare element and we would not exist! ...
... because carbon nuclei have an energy level at exactly the right place otherwise carbon would be a rare element and we would not exist! ...
The Formation of Low Mass Stars: Overview and Recent
... Sequence of Bonnor-Ebert spheres of increasing nc e.g., Shu (1977) “Inside-out collapse” ...
... Sequence of Bonnor-Ebert spheres of increasing nc e.g., Shu (1977) “Inside-out collapse” ...
Stellar Luminosity and Mass Functions * * * * * History and
... If protogalactic clouds merge dissipatively in a potential well of a dark halo, they will settle in a thin, rotating disk = the minimum energy configuration for a given angular momentum. If gas settles into a (dynamically cold) disk before stars form, then stars formed in that disk will inherit the ...
... If protogalactic clouds merge dissipatively in a potential well of a dark halo, they will settle in a thin, rotating disk = the minimum energy configuration for a given angular momentum. If gas settles into a (dynamically cold) disk before stars form, then stars formed in that disk will inherit the ...
Clase-06_Star_Formation - Departamento de Astronomía
... free e- pressure starts to balance the collapse that eventually halts in the core convective proto-star reachs the Hayashi limit in the CM diagram and enter the hydrostatic equilibrium regime (becoming a T-Tauri star) the core starts to burn D and Li and becomes radiative, the envelope continu ...
... free e- pressure starts to balance the collapse that eventually halts in the core convective proto-star reachs the Hayashi limit in the CM diagram and enter the hydrostatic equilibrium regime (becoming a T-Tauri star) the core starts to burn D and Li and becomes radiative, the envelope continu ...
5.3 Convective transport
... is fast enough for the parcel not to exchange heat with its surroundings, while at the same time having time to get into pressure equilibrium. These assumptions might not seem very realistic, so we will see if they are realistic ...
... is fast enough for the parcel not to exchange heat with its surroundings, while at the same time having time to get into pressure equilibrium. These assumptions might not seem very realistic, so we will see if they are realistic ...
The lifes of a star
... Recall that all atoms are made of a very dense and small nucleus which is positively charged and a bunch of electrons, which are negatively charged, and which surround the nucleus. At the center of the stars temperatures as very high (at least a few million degrees Celsius); pressures are also high ...
... Recall that all atoms are made of a very dense and small nucleus which is positively charged and a bunch of electrons, which are negatively charged, and which surround the nucleus. At the center of the stars temperatures as very high (at least a few million degrees Celsius); pressures are also high ...
Stellar Evolution
... result, when fragmentation to stellar-mass sizes occur, each little cloudlet has a rotation associated with it that was induced from one of these eddies as shown in Figure II-5. 3. As the cloudlet contracts, it spins faster due to the conservation of angular momentum L = M R2 ω, where ω is the angul ...
... result, when fragmentation to stellar-mass sizes occur, each little cloudlet has a rotation associated with it that was induced from one of these eddies as shown in Figure II-5. 3. As the cloudlet contracts, it spins faster due to the conservation of angular momentum L = M R2 ω, where ω is the angul ...
Star Formation in Our Galaxy - Wiley-VCH
... nearby stars into our direction.2 The mid- and far-infrared emission from warm dust particles provides yet another means to study the Orion region. The first instrument devoted exclusively to infrared mapping of the sky was IRAS (for Infrared Astronomical Satellite), launched in 1983. Figure 1.4, wh ...
... nearby stars into our direction.2 The mid- and far-infrared emission from warm dust particles provides yet another means to study the Orion region. The first instrument devoted exclusively to infrared mapping of the sky was IRAS (for Infrared Astronomical Satellite), launched in 1983. Figure 1.4, wh ...
A Stars
... • B Stars (15-30,000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): Ideal excitation conditions, strongest H lines. • G Stars (6000 K): Too cool, little excited H, so only weak H lines. ...
... • B Stars (15-30,000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): Ideal excitation conditions, strongest H lines. • G Stars (6000 K): Too cool, little excited H, so only weak H lines. ...
Introduction: The Night Sky
... helium fusion lasts around one million years carbon fusion lasts 300 years oxygen fusion lasts for 7 months silicon fusion lasts for two days and produces an iron core ...
... helium fusion lasts around one million years carbon fusion lasts 300 years oxygen fusion lasts for 7 months silicon fusion lasts for two days and produces an iron core ...
Hvězdný make up Proč jsou hvězdy skvrnité?
... Assuming magnetic field of tepid MS stars is fossil one → all photospheres should be in some extent controlled by magnetic field → transient spot structures on even ‘normal’ (non-CP) tepid MS stars are allowed. ...
... Assuming magnetic field of tepid MS stars is fossil one → all photospheres should be in some extent controlled by magnetic field → transient spot structures on even ‘normal’ (non-CP) tepid MS stars are allowed. ...
Chapter12 (with interactive links)
... Evolution in Close Binary Systems: The White Dwarf Limit (Cont.) ...
... Evolution in Close Binary Systems: The White Dwarf Limit (Cont.) ...
Chandra and NIR Observations of Galactic HII Regions
... many nearby O stars whose winds are thought to drive instabilities and X-ray emitting shocks. • The O stars in NGC 6611 are to be contrasted with those in the younger Orion Nebula Cluster with hard, time-variable X-rays and higher LX/Lbol, most likely produced by magnetic activity. ...
... many nearby O stars whose winds are thought to drive instabilities and X-ray emitting shocks. • The O stars in NGC 6611 are to be contrasted with those in the younger Orion Nebula Cluster with hard, time-variable X-rays and higher LX/Lbol, most likely produced by magnetic activity. ...
Stellar Winds and Supernova Remnants: Interaction with the ISM
... IRC+10216 showing shell-like structures in the circumstellar envelope (90''x 90'') Mauron & Huggins (2010) ...
... IRC+10216 showing shell-like structures in the circumstellar envelope (90''x 90'') Mauron & Huggins (2010) ...
galaxies and stars
... less luminous and have a lower surface temperature less luminous and have a higher surface temperature more luminous and have a lower surface temperature more luminous and have a higher surface temperature ...
... less luminous and have a lower surface temperature less luminous and have a higher surface temperature more luminous and have a lower surface temperature more luminous and have a higher surface temperature ...
From galaxies to stars
... These disks will eventually be where planets form. In the meantime, the protostar is continuing to contract and heat up. Eventually, the temperature in the core of the star becomes hot enough that hydrogen can fuse to form helium, just as it did in the first three minutes after the Big Bang. This f ...
... These disks will eventually be where planets form. In the meantime, the protostar is continuing to contract and heat up. Eventually, the temperature in the core of the star becomes hot enough that hydrogen can fuse to form helium, just as it did in the first three minutes after the Big Bang. This f ...
Angular momentum evolution
... • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and brown dwarfs ...
... • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and brown dwarfs ...
0.1 Chapter 2
... Answer: By local thermodynamic equilibrium, we mean that a region of a star with size much smaller than the radius of that star, but larger than the mean free path of photons, there is a well defined local temperature. This means that in the star there is a well defined temperature distribution. The ...
... Answer: By local thermodynamic equilibrium, we mean that a region of a star with size much smaller than the radius of that star, but larger than the mean free path of photons, there is a well defined local temperature. This means that in the star there is a well defined temperature distribution. The ...
Gravitational Waves from Neutron Stars
... Gravitational waves from newly born, hot neutron stars V. Ferrari, G. Miniutti, J. Pons, MNRAS 2003, to appear ...
... Gravitational waves from newly born, hot neutron stars V. Ferrari, G. Miniutti, J. Pons, MNRAS 2003, to appear ...