Our Worlds, Other Worlds
... Scientists have discovered that most of the heavy elements in the universe are dispersed from stars that go supernova. ...
... Scientists have discovered that most of the heavy elements in the universe are dispersed from stars that go supernova. ...
Understanding HF propagation
... 5. The solar wind • The solar wind originates from the solar corona, the outermost visible area in the sun. The corona is so hot that the atoms there cannot remain as atoms but they get ionized. That is why the solar wind is almost 100% ionized plasma, containing mainly protons and electrons. • The ...
... 5. The solar wind • The solar wind originates from the solar corona, the outermost visible area in the sun. The corona is so hot that the atoms there cannot remain as atoms but they get ionized. That is why the solar wind is almost 100% ionized plasma, containing mainly protons and electrons. • The ...
Are we there yet? A Journey to Understand and Predict Solar
... Abrupt increase in radiative output at all wavelengths ...
... Abrupt increase in radiative output at all wavelengths ...
Chapter 11
... wind, a tenuous gas of hydrogen and helium that sweeps across the entire Solar System • The amount of material lost from the Sun via the Solar Wind is insignificant • Typical values at the Earth’s orbit: a few atoms per cm3 and a speed of about 500 km/sec • At some point, the solar wind mingles with ...
... wind, a tenuous gas of hydrogen and helium that sweeps across the entire Solar System • The amount of material lost from the Sun via the Solar Wind is insignificant • Typical values at the Earth’s orbit: a few atoms per cm3 and a speed of about 500 km/sec • At some point, the solar wind mingles with ...
AH Additional notes on stellar physics
... As the power per unit area is proportional to T 4 , this means that as temperature rises the quantity of radiation emitted per unit area increases very rapidly. However, radiation is not emitted at a single wavelength but over a characteristic waveband, as shown in Figure 9. This diagram is called a ...
... As the power per unit area is proportional to T 4 , this means that as temperature rises the quantity of radiation emitted per unit area increases very rapidly. However, radiation is not emitted at a single wavelength but over a characteristic waveband, as shown in Figure 9. This diagram is called a ...
Stellar Physics - support material
... As the power per unit area is proportional to T 4 , this means that as temperature rises the quantity of radiation emitted per unit area increases very rapidly. However, radiation is not emitted at a single wavelength but over a characteristic waveband, as shown in Figure 9. This diagram is called a ...
... As the power per unit area is proportional to T 4 , this means that as temperature rises the quantity of radiation emitted per unit area increases very rapidly. However, radiation is not emitted at a single wavelength but over a characteristic waveband, as shown in Figure 9. This diagram is called a ...
free magnetic energy and flare productivity of active
... three produced major flares (X- and/or M-class). To check the statistical correlation between Efree and FIn−day , it is important that the sample is comprised major flaring, moderate flaring, and flare-quiet regions. Therefore, we give priority to NOAA 10930 and 10960, as they are two of the very fe ...
... three produced major flares (X- and/or M-class). To check the statistical correlation between Efree and FIn−day , it is important that the sample is comprised major flaring, moderate flaring, and flare-quiet regions. Therefore, we give priority to NOAA 10930 and 10960, as they are two of the very fe ...
The Sun - Humble ISD
... At one end of the loop, the breakthrough point is a magnetic north pole. At this point, the direction of the field lines is upward -- that is, Magnetic field away from the interior. At the other end of the loop, the breakthrough point is a magnetic south Some of the time, the sun's magnetic field ha ...
... At one end of the loop, the breakthrough point is a magnetic north pole. At this point, the direction of the field lines is upward -- that is, Magnetic field away from the interior. At the other end of the loop, the breakthrough point is a magnetic south Some of the time, the sun's magnetic field ha ...
Research with Space Weather Monitor Data
... structure costing little and taking a few hours to assemble. Data collection and analysis is handled by a local PC, which need not be fast or elaborate. Stanford provides a centralized data repository and blog site where students can exchange and discuss data. Two versions of the monitor exist - one ...
... structure costing little and taking a few hours to assemble. Data collection and analysis is handled by a local PC, which need not be fast or elaborate. Stanford provides a centralized data repository and blog site where students can exchange and discuss data. Two versions of the monitor exist - one ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... - Non-equilibrium ionization (seen in the sun, locally-flares) may be a bigger issue in wind-shock sources, where the plasma is moving rapidly…recombination and cooling times are of order 103 to 104 seconds, as are flow times. - Excitation out of excited states can be important for metastable levels ...
... - Non-equilibrium ionization (seen in the sun, locally-flares) may be a bigger issue in wind-shock sources, where the plasma is moving rapidly…recombination and cooling times are of order 103 to 104 seconds, as are flow times. - Excitation out of excited states can be important for metastable levels ...
what sets the initial rotation rates of massive stars?
... formation theory. Observations of young, massive stars provide evidence that they form in a similar fashion to their low-mass counterparts. The magnetic coupling between a star and its accretion disk may be sufficient to spin down low-mass pre-main-sequence (PMS) stars to well below breakup at the e ...
... formation theory. Observations of young, massive stars provide evidence that they form in a similar fashion to their low-mass counterparts. The magnetic coupling between a star and its accretion disk may be sufficient to spin down low-mass pre-main-sequence (PMS) stars to well below breakup at the e ...
Gamma-ray emission from Wolf
... In this paper we will study the case of three WR binaries: WR 140, WR 146, and WR 147. We will use the most recent results from radio observations in order to fix the value of model parameters, and then we will compute the expected gammaray luminosity with reasonable assumptions for the magnetic fie ...
... In this paper we will study the case of three WR binaries: WR 140, WR 146, and WR 147. We will use the most recent results from radio observations in order to fix the value of model parameters, and then we will compute the expected gammaray luminosity with reasonable assumptions for the magnetic fie ...
High-latitude electrojets, auroral luminosity and auroral
... precipitation of energetic particle fluxes into the upper atmosphere. The magnetic disturbances are of the highest intensity in the auroral region, becoming less intense poleward and at subauroral latitudes. The irregular character of geomagnetic field disturbances was mentioned by Birkeland [1908], ...
... precipitation of energetic particle fluxes into the upper atmosphere. The magnetic disturbances are of the highest intensity in the auroral region, becoming less intense poleward and at subauroral latitudes. The irregular character of geomagnetic field disturbances was mentioned by Birkeland [1908], ...
Electric current in flares ribbons: observations and 3D standard model
... HMI/SDO magnetic observations and find that localized currents in J-shaped ribbons increase to double their pre-flare intensity. Our 3D flare model, developed with the OHM code, suggests that these current ribbons, which develop at the location of EUV brightenings seen with AIA imagery, are driven b ...
... HMI/SDO magnetic observations and find that localized currents in J-shaped ribbons increase to double their pre-flare intensity. Our 3D flare model, developed with the OHM code, suggests that these current ribbons, which develop at the location of EUV brightenings seen with AIA imagery, are driven b ...
Global auroral responses to abrupt solar wind changes: Dynamic
... fundamental response types. For not strongly southward IMF conditions (Bz ^ 5 nT), we find that IMF changes that are expected to reduce the convection electric field after ^30 min of negative IMF Bz cause typical substorms, where expansion phase auroral activity initiates within the expected locati ...
... fundamental response types. For not strongly southward IMF conditions (Bz ^ 5 nT), we find that IMF changes that are expected to reduce the convection electric field after ^30 min of negative IMF Bz cause typical substorms, where expansion phase auroral activity initiates within the expected locati ...
STRUCTURE AND EVOLUTION OF WHITE DWARFS S. 0. Kepler1
... DA white dwarfs. The radius for a given mass is larger at higher temperature and slowly approaches the zero-temperature value. Bergeron et al. (1995a) derive an average mass of about 0.60 M©, and the spectroscopic and gravitational redshift average masses agree to better than 0.05 AT© for all subset ...
... DA white dwarfs. The radius for a given mass is larger at higher temperature and slowly approaches the zero-temperature value. Bergeron et al. (1995a) derive an average mass of about 0.60 M©, and the spectroscopic and gravitational redshift average masses agree to better than 0.05 AT© for all subset ...
