Indirect Observation Method - Portal do Professor
... because their “filters of reality” and expectations are distinct. It means that the subjective reality of the observer can lead to different procedures and result in a different “objective” reality for the observer. This curious phenomenon has been observed in the most diverse scientific fields, suc ...
... because their “filters of reality” and expectations are distinct. It means that the subjective reality of the observer can lead to different procedures and result in a different “objective” reality for the observer. This curious phenomenon has been observed in the most diverse scientific fields, suc ...
Fingerprints-in-Sunlight
... The Sun emits a continuous spectrum All light from the Sun comes from the surface, or photosphere, 5800 degrees K As the atoms bounce around the photosphere, photons are constantly being absorbed and re-emitted Although the original light was traveling our way, re-emitted photons are sent off in all ...
... The Sun emits a continuous spectrum All light from the Sun comes from the surface, or photosphere, 5800 degrees K As the atoms bounce around the photosphere, photons are constantly being absorbed and re-emitted Although the original light was traveling our way, re-emitted photons are sent off in all ...
letters - MIT Kavli Institute for Astrophysics and Space Research
... find for nearby stars. These higher Ne/O ratios were obtained for hotter active regions13,20 that are likely to dominate the solar full-disk X-ray emission. These measurements are the most directly compatible with the ones presented here based on full-disk integrated light X-ray spectra of stars. Si ...
... find for nearby stars. These higher Ne/O ratios were obtained for hotter active regions13,20 that are likely to dominate the solar full-disk X-ray emission. These measurements are the most directly compatible with the ones presented here based on full-disk integrated light X-ray spectra of stars. Si ...
talk - University of Southampton
... Blandford-Znajek effect When free charges are introduced this field can sustain electric currents along the field lines penetrating the black hole ergosphere. For the perfectly conducting case with insignificant inertia of plasma the magnetosphere is described by Magnetodynamics (MD -- inertia-free ...
... Blandford-Znajek effect When free charges are introduced this field can sustain electric currents along the field lines penetrating the black hole ergosphere. For the perfectly conducting case with insignificant inertia of plasma the magnetosphere is described by Magnetodynamics (MD -- inertia-free ...
DR The Sun File
... a. 25% of 1,390 km b. 25% of 13,900 km c. 25% of 139,000 km d. 25% of 1,390,000 km 56. What is the sun’s core made up of? ______________________________________________________________ 57. How does the mass of the sun compare with the mass of Earth? __________________________________________________ ...
... a. 25% of 1,390 km b. 25% of 13,900 km c. 25% of 139,000 km d. 25% of 1,390,000 km 56. What is the sun’s core made up of? ______________________________________________________________ 57. How does the mass of the sun compare with the mass of Earth? __________________________________________________ ...
Chapter 13
... B) all pulsars must have their poles pointed directly toward us. C) the period of pulsation slows down due to the drag of the remnant on its field. D) the star literally turns on and off like a lighthouse beacon. E) if the beam sweeps across us, we will detect a pulse of radiation. 11. Neutron stars ...
... B) all pulsars must have their poles pointed directly toward us. C) the period of pulsation slows down due to the drag of the remnant on its field. D) the star literally turns on and off like a lighthouse beacon. E) if the beam sweeps across us, we will detect a pulse of radiation. 11. Neutron stars ...
Formation of Solar System
... Why did this mass come together? What triggered this process? Here there is no clear answer – Perhaps a shock wave from a supernova or some other event. ...
... Why did this mass come together? What triggered this process? Here there is no clear answer – Perhaps a shock wave from a supernova or some other event. ...
How does the solar wind blow? A simple kinetic model
... The starting point of the kinetic description is as follows: at the distance where the particles are free to escape since the gravitational binding energy there becomes smaller than the thermal energy, the mean-free path has already become greater than the scale height, so that the medium is no long ...
... The starting point of the kinetic description is as follows: at the distance where the particles are free to escape since the gravitational binding energy there becomes smaller than the thermal energy, the mean-free path has already become greater than the scale height, so that the medium is no long ...
Our Sun, Sol - Hobbs High School
... activity are sunspots, solar flares, and solar prominences. ...
... activity are sunspots, solar flares, and solar prominences. ...
Supernovae
... Supernovae occur at the end of the evolutionary history of stars. The star must be at least 2 solar masses: the core at least 1.4 solar masses. Stellar core collapses under force of its own gravitation. Energy set free by collapse expels most of star’s mass. A dense remnant, often a neutron star, is ...
... Supernovae occur at the end of the evolutionary history of stars. The star must be at least 2 solar masses: the core at least 1.4 solar masses. Stellar core collapses under force of its own gravitation. Energy set free by collapse expels most of star’s mass. A dense remnant, often a neutron star, is ...
Radio Detection of Extrasolar Planets:
... Emission weak – probably beyond current capabilities even with variability; Beaming increases the flux density, but decreases the probabilit y of detection concomitantly; Difficult to disentangle detected emission from that of the star (periodicity is a key to resolving this ambiguity); For planets ...
... Emission weak – probably beyond current capabilities even with variability; Beaming increases the flux density, but decreases the probabilit y of detection concomitantly; Difficult to disentangle detected emission from that of the star (periodicity is a key to resolving this ambiguity); For planets ...
Our Star, the Sun
... A Neutrino coming out of this reaction means that it is govern by the weak nuclear force so it’s weak and slow which disproves this whole formula o Step 2: Proton + Deuteron Helium 3 Nucleus + High energy photon (gamma ray) o Step 3: Helium 3 + Helium 3 Helium 4 and some protons o Simplificati ...
... A Neutrino coming out of this reaction means that it is govern by the weak nuclear force so it’s weak and slow which disproves this whole formula o Step 2: Proton + Deuteron Helium 3 Nucleus + High energy photon (gamma ray) o Step 3: Helium 3 + Helium 3 Helium 4 and some protons o Simplificati ...
The Sun The Sun
... takes about 8 minutes to reach Earth, even though light travels incredibly fast. When we see the Sun, we’re really seeing what it looked like 8 minutes ago. How Hot Is the Sun? The temperature of the Sun can reach 5,500ºC (10,000ºF) on the surface and more than 15.5 million ºC (28 million ºF) at the ...
... takes about 8 minutes to reach Earth, even though light travels incredibly fast. When we see the Sun, we’re really seeing what it looked like 8 minutes ago. How Hot Is the Sun? The temperature of the Sun can reach 5,500ºC (10,000ºF) on the surface and more than 15.5 million ºC (28 million ºF) at the ...
SDO Systems Retreat
... 2. Provide information about the global solar magnetic field, the active region evolution, small-scale features, and sources of irradiance variations. (Longitudinal and Vector Magnetic Field Images, Atmospheric Images, Spectral Irradiance Measurements) 3. Characterize the rapid evolution of plasma i ...
... 2. Provide information about the global solar magnetic field, the active region evolution, small-scale features, and sources of irradiance variations. (Longitudinal and Vector Magnetic Field Images, Atmospheric Images, Spectral Irradiance Measurements) 3. Characterize the rapid evolution of plasma i ...
ES_CH3_L1 - AFJROTC Ar/Ld 4
... The Sun provides the light, heat and energy that make life on Earth possible In order for the Sun to produce its enormous power, a large number of fusions of hydrogen nuclei must take place every second The three layers of the Sun’s atmosphere are photosphere, chromosphere, and ...
... The Sun provides the light, heat and energy that make life on Earth possible In order for the Sun to produce its enormous power, a large number of fusions of hydrogen nuclei must take place every second The three layers of the Sun’s atmosphere are photosphere, chromosphere, and ...
(1) and
... Kinematic energy (=1/2Mv2) of Ia and CC SN are ~1051 erg. A large fraction should be converted to the thermal energy: kT = 3mv2/16 However observed thermal energy (kTe) is ~1049 erg This large missing energy would be contained in protons and other ions (the ion temperature kTi). But, no evidence is ...
... Kinematic energy (=1/2Mv2) of Ia and CC SN are ~1051 erg. A large fraction should be converted to the thermal energy: kT = 3mv2/16 However observed thermal energy (kTe) is ~1049 erg This large missing energy would be contained in protons and other ions (the ion temperature kTi). But, no evidence is ...
PPT
... Interplanetary CMEs may exhibit three relevant radio emission mechanisms: bremsstrahlung, gyrosynchrotron emission and plasma emission. Bremsstrahlung is produced by Coulomb collisions between charged particles in plasmas. Gyrosynchrotron emission is the electromagnetic emission generated by mildly ...
... Interplanetary CMEs may exhibit three relevant radio emission mechanisms: bremsstrahlung, gyrosynchrotron emission and plasma emission. Bremsstrahlung is produced by Coulomb collisions between charged particles in plasmas. Gyrosynchrotron emission is the electromagnetic emission generated by mildly ...
Abundances - Michigan State University
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
Solarnet III / HELAS VII / SpaceInn 2015 funded - science
... • Fostering scientific exchange and synergies between these two areas of astrophysics • Reviewing both areas: ...
... • Fostering scientific exchange and synergies between these two areas of astrophysics • Reviewing both areas: ...
High Energy Processes in Young Stellar Objects
... Field lines above corotation radius Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
... Field lines above corotation radius Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
Gravitational Collapse
... enough, H atoms can form H2. Unfortunately, no emission from H2 in the optical or radio bands. Therefore use, 1. Other molecules. For example, CO emits radiation at a wavelength of 2.6mm microwaves. 2. Dust. Dust (and molecules) are often found together - dense, dark clouds (called Bok globules) are ...
... enough, H atoms can form H2. Unfortunately, no emission from H2 in the optical or radio bands. Therefore use, 1. Other molecules. For example, CO emits radiation at a wavelength of 2.6mm microwaves. 2. Dust. Dust (and molecules) are often found together - dense, dark clouds (called Bok globules) are ...
Stellar Evolution
... of a dying, sun-like star.” • “The hourglass shapes of many planetary nebulae are produced by the expansion of a ‘fast stellar wind’ within a slowly expanding ’cloud’ which is denser near its equator than its poles.” • If so, where do the x-rays come from? ...
... of a dying, sun-like star.” • “The hourglass shapes of many planetary nebulae are produced by the expansion of a ‘fast stellar wind’ within a slowly expanding ’cloud’ which is denser near its equator than its poles.” • If so, where do the x-rays come from? ...
Homework #4 (Ch. 16)
... rays. Because the gas in the core is totally ionized, it is transparent to radiation and so the radiation passes through it freely. But as we get closer to the surface, the temperature drops, and more and more of the gas is not ionized or only partially ionized. Such a gas is opaque to radiation. At ...
... rays. Because the gas in the core is totally ionized, it is transparent to radiation and so the radiation passes through it freely. But as we get closer to the surface, the temperature drops, and more and more of the gas is not ionized or only partially ionized. Such a gas is opaque to radiation. At ...
Acoustic Waves - The Evergreen State College
... and pressure gradients. In Alfvén waves the field E1 is perpendicular to the direction of propagation k and velocity perturbation v1 of the wave (Fig. 9). In magnetosonic waves the field E1 is perpendicular to k and parallel to v1. In acoustic waves, the pressure gradient is antiparallel to the elec ...
... and pressure gradients. In Alfvén waves the field E1 is perpendicular to the direction of propagation k and velocity perturbation v1 of the wave (Fig. 9). In magnetosonic waves the field E1 is perpendicular to k and parallel to v1. In acoustic waves, the pressure gradient is antiparallel to the elec ...
Corona
A corona (Latin, 'crown') is an aura of plasma that surrounds the sun and other celestial bodies. The Sun's corona extends millions of kilometres into space and is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The word ""corona"" is a Latin word meaning ""crown"", from the Ancient Greek κορώνη (korōnē, “garland, wreath”).The high temperature of the Sun's corona gives it unusual spectral features, which led some in the 19th century to suggest that it contained a previously unknown element, ""coronium"". Instead, these spectral features have since been explained by highly ionized iron (Fe-XIV). Bengt Edlén, following the work of Grotrian (1939), first identified the coronal lines in 1940 (observed since 1869) as transitions from low-lying metastable levels of the ground configuration of highly ionised metals (the green Fe-XIV line at 5303 Å, but also the red line Fe-X at 6374 Å). These high stages of ionisation indicate a plasma temperature in excess of 1,000,000 kelvin, much hotter than the surface of the sun.Light from the corona comes from three primary sources, which are called by different names although all of them share the same volume of space. The K-corona (K for kontinuierlich, ""continuous"" in German) is created by sunlight scattering off free electrons; Doppler broadening of the reflected photospheric absorption lines completely obscures them, giving the spectral appearance of a continuum with no absorption lines. The F-corona (F for Fraunhofer) is created by sunlight bouncing off dust particles, and is observable because its light contains the Fraunhofer absorption lines that are seen in raw sunlight; the F-corona extends to very high elongation angles from the Sun, where it is called the zodiacal light. The E-corona (E for emission) is due to spectral emission lines produced by ions that are present in the coronal plasma; it may be observed in broad or forbidden or hot spectral emission lines and is the main source of information about the corona's composition.