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How much radioactive nickel does ASASSN
How much radioactive nickel does ASASSN

Bellwork: Degenerate Matter (A review form yesterday)
Bellwork: Degenerate Matter (A review form yesterday)

... particles are arranged in energy levels like rungs of an energy ladder. In ordinary gas, most of the energy levels are unfilled and the particles are free to move about. But in a degenerate gas, all of the lower energy levels are filled. The second rule is that only two particles can share the same ...
Black Hole Accretion
Black Hole Accretion

... Each argument has loopholes (hardly any for bursts) If BHCs are not black holes, they must negotiate so many different constraints, it becomes highly ...
are coronae of late-type stars made of solar-like structures? the x
are coronae of late-type stars made of solar-like structures? the x

... coronal activity, albeit averaged over the whole corona. Indeed, FX gives the coronal radiative losses of the star per unit area and is related to the amount of energy delivered into the corona, i.e., the coronal heating, also per unit area. It can discriminate between two stars of the same X-ray lu ...
IMAP (Interstellar MApping Probe)
IMAP (Interstellar MApping Probe)

SUPERNOVA EMISSION FROM GAMMA RAYS TO THE INFRARED
SUPERNOVA EMISSION FROM GAMMA RAYS TO THE INFRARED

... We have shown by modeling of the 1987A spectrum  at 8 years (Jerkstrand et al, in prep.) and 20 years  (Kjaer et al 2010, in press), that ~1*10­4 Msun of 44Ti  is powering the deepest core regions in the  supernova, producing emission in newly synthesized  iron, silicon and oxygen. ...
CME - ASU
CME - ASU

... They did not account for ordinary stellar wind ...
EIS 1 Our Ideas About Space
EIS 1 Our Ideas About Space

... A. *What is responsible for the length of 1 day? Earth rotating on its axis is responsible for the length of a day. *What is responsible for the length of 1 year? The orbit around the Sun is responsible for the length of a year. B. What causes seasons? The distance from Earth to the Sun as it rotate ...
4. Star Formation
4. Star Formation

... – at densities of 1011 cm−3 and at a radius of 1014 cm the gas becomes optically thick for dust radiation at even 300µ m. Hence, energy is trapped and the temperature rises; increasing temperature increases opacity further; collapse turns adiabatic – The high thermal pressure resists gravity and end ...
What constitutes the dark matter?
What constitutes the dark matter?

... More than 2000 objects with earth mass observed in microlensing ...
SRC and the fate of cold neutron stars
SRC and the fate of cold neutron stars

Our Earth in space
Our Earth in space

... A group of stars is called a GALAXY. Our sun is part of a galaxy called the MILKY WAY. The Universe is made up of many such galaxies. The Earth is a PLANET. The planets do NOT give out their own light but reflect the light from the sun. The planets are in ORBIT around the sun. This means they go aro ...
protostellar disks under the influence of winds and uv radiation
protostellar disks under the influence of winds and uv radiation

... radiation. The central stars themselves can have a stellar wind and may produce sufficient UV and X-ray to ultimately destroy their surrounding disks. Here we describe the results of numerical simulations of the influence that an external UV source and a central star’s wind can have on its circumste ...
Colour and Luminosity Trends from the 6dFGS
Colour and Luminosity Trends from the 6dFGS

Dark Matter: Inquiring Minds Want to Know ()
Dark Matter: Inquiring Minds Want to Know ()

... from things like stars • Can see the light from stars AFTER it has left the star and interacted with whatever is between us and the star ...
The VLSR Correction - Johns Hopkins University
The VLSR Correction - Johns Hopkins University

Flares and the chromosphere Hugh S. Hudson and Lyndsay Fletcher
Flares and the chromosphere Hugh S. Hudson and Lyndsay Fletcher

... The observations indicate that coronal energy dissipates in the chromosphere, and the hard X-ray signature directly implicates weakly relativistic electrons. Thus the magnetic restructuring, and the energy transport it implies, must somehow result in the acceleration of electrons to non-thermal ener ...
SECOND SUN - royal device
SECOND SUN - royal device

Chapter 1 The Scale of the Cosmos: From Solar System to Galaxy to
Chapter 1 The Scale of the Cosmos: From Solar System to Galaxy to

General Module information
General Module information

... Explain qualitatively how the equation of state is modified by radiation pressure. Explain qualitatively what is meant by radiative transfer. Explain qualitatively the effects of turbulence in stellar atmospheres. ...
(massive) binary stars
(massive) binary stars

... showed that neither the vsini nor rotational frequency of a massive star have predictive power for the surface nitrogen abundance. Instead, there is a clear correlation between the effective temperature/the dominant acoustic oscillation mode of a star and atmospheric nitrogen abundance. With this pr ...
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... planets in solar system wrt Earth-Sun 1 AU. • Measure parallax of Earth-Sun, Earth-Planets etc • Observe from one side of Earth to other ...
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Heavy elements game

3.2 Gravity and the Solar System
3.2 Gravity and the Solar System

PDF Full-text
PDF Full-text

... the photodissociation rate for H2 O in exoplanets with solar-type and M dwarf host stars including the observed UV fluxes and Lyman-α corrected for interstellar absorption to evaluate the H2 O loss rate. At this time, however, there are very few disequilibrium chemistry calculations that include obs ...
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Standard solar model

The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma). This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined. The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System. The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium. All heavier elements, called metals in astronomy, account for less than 2 percent of the mass. The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to ""fit"" the observed Sun.
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