Power Point Presentation
... filament activation in a solar eruption, submitted to Astron. & Astrophys., 2011 11. Rubio da Costa, F., Zuccarello, F., Romano, P., Fletcher, L., Labrosse, N., Relationship between an M6.6 solar flare and consecutive filament activations, Mem. S.A.It. in press, 2011 12. Rubio da Costa, F., Zuccarel ...
... filament activation in a solar eruption, submitted to Astron. & Astrophys., 2011 11. Rubio da Costa, F., Zuccarello, F., Romano, P., Fletcher, L., Labrosse, N., Relationship between an M6.6 solar flare and consecutive filament activations, Mem. S.A.It. in press, 2011 12. Rubio da Costa, F., Zuccarel ...
Chapter 5 The Solar Wind
... the ecliptic and highly warped. During periods of solar minimum the interplanetary field seen at the Earth is dominated by two recurring sectors (one toward, one away) per solar rotation. During periods of maximum activity, the IMF is much more complex, with four or more recognisable sectors and man ...
... the ecliptic and highly warped. During periods of solar minimum the interplanetary field seen at the Earth is dominated by two recurring sectors (one toward, one away) per solar rotation. During periods of maximum activity, the IMF is much more complex, with four or more recognisable sectors and man ...
ALLAN SACHA BRUN Head of the Laboratory on Dynamics
... - Assessed the respective role of Reynolds, Maxwell stresses, meridional circulation or viscous effects. Extended analysis to other stars such A, F, K , T Tauri’s or low mass RGB stars. - Developed a 2--D finite element axisymmetric MHD code STELEM to study the solar and stellar magnetic cycles, bu ...
... - Assessed the respective role of Reynolds, Maxwell stresses, meridional circulation or viscous effects. Extended analysis to other stars such A, F, K , T Tauri’s or low mass RGB stars. - Developed a 2--D finite element axisymmetric MHD code STELEM to study the solar and stellar magnetic cycles, bu ...
55_1.pdf
... Sun’s magnetism from density structure observed in whitelight images. Polar plumes, the small-scale, faint, thin, hair-like structures resembling the lines of force of a bar magnet, suggest that polar coronal holes are the source of open field lines (1). The abundance of photospheric magnetograms ma ...
... Sun’s magnetism from density structure observed in whitelight images. Polar plumes, the small-scale, faint, thin, hair-like structures resembling the lines of force of a bar magnet, suggest that polar coronal holes are the source of open field lines (1). The abundance of photospheric magnetograms ma ...
China Power Investment Opts for High-Quality, Field
... wind can take a heavy toll and solar panels endure harsh ultraviolet rays and thermal stress. Sharing expertise is also part of the DuPont/CPI relationship. For CPI, expanding on its original emphasis on hydroelectric to include new wind and solar power projects, having access to the knowledge base ...
... wind can take a heavy toll and solar panels endure harsh ultraviolet rays and thermal stress. Sharing expertise is also part of the DuPont/CPI relationship. For CPI, expanding on its original emphasis on hydroelectric to include new wind and solar power projects, having access to the knowledge base ...
A Study on Midrange Periodicity of Sunspot Number During Solar
... 10.3 years, beginning in 1976 and ending in 1986. The maximum smoothed sunspot number (monthly number of sunspots averaged over a twelve month period) observed during the solar cycle was 164.5, and the minimum was 12.3.There were a total of 273 days with no sunspots during this cycle. Solar cycle 22 ...
... 10.3 years, beginning in 1976 and ending in 1986. The maximum smoothed sunspot number (monthly number of sunspots averaged over a twelve month period) observed during the solar cycle was 164.5, and the minimum was 12.3.There were a total of 273 days with no sunspots during this cycle. Solar cycle 22 ...
Determination of a Correlation of Sunspot Number and 20.1 MHz
... alongside sunspot number versus time were created. Based on what we know of the physics behind sunspots and solar bursts, the data agrees with the theory to a considerable degree. Based on this result we expect the solar burst number to increase as more sunspots are seen. ...
... alongside sunspot number versus time were created. Based on what we know of the physics behind sunspots and solar bursts, the data agrees with the theory to a considerable degree. Based on this result we expect the solar burst number to increase as more sunspots are seen. ...
AAS_WFXT_Solar_System_11Jan2010
... the course of the mission. WFXT will thus be a bonanza for solar system x-ray astrophysics. Understanding local soft xray emission processes, driven by scattering of solar x-rays and charge exchange with the solar wind, means understanding the nearest, best example of a stellar wind throughout inter ...
... the course of the mission. WFXT will thus be a bonanza for solar system x-ray astrophysics. Understanding local soft xray emission processes, driven by scattering of solar x-rays and charge exchange with the solar wind, means understanding the nearest, best example of a stellar wind throughout inter ...
Signatures of stellar surface structure
... Predicted (solid) and observed bisectors for differently strong solar lines; 3-D hydrodynamic modeling on an absolute velocity scale. (Classical 1D models produce vertical bisectors at zero absolute velocity.) M.Asplund, Å.Nordlund, R.Trampedach, C.Allende Prieto, R.F.Stein: Line formation in solar ...
... Predicted (solid) and observed bisectors for differently strong solar lines; 3-D hydrodynamic modeling on an absolute velocity scale. (Classical 1D models produce vertical bisectors at zero absolute velocity.) M.Asplund, Å.Nordlund, R.Trampedach, C.Allende Prieto, R.F.Stein: Line formation in solar ...
SolarGrandMinimaThreat Analysis
... Variations in the amount of sunlight reaching the oceans control the rate at which the oceans warm. This is influenced at long time scales by changes in the Earth’s orbit. At short time scales there are changes in the amount of solar irradiance associated with the sunspot cycle. These changes are sm ...
... Variations in the amount of sunlight reaching the oceans control the rate at which the oceans warm. This is influenced at long time scales by changes in the Earth’s orbit. At short time scales there are changes in the amount of solar irradiance associated with the sunspot cycle. These changes are sm ...
Formation of Solar System
... – Dense clouds litter the galaxy – Low temperature (10 K) – High density (1000 to 1 million times greater than interstellar medium) – Rich collection of molecules (but mostly H) – 1015 km in diameter – 2000 or so in Milky Way – Favorable places for star formation (and, therefore, perhaps planetary f ...
... – Dense clouds litter the galaxy – Low temperature (10 K) – High density (1000 to 1 million times greater than interstellar medium) – Rich collection of molecules (but mostly H) – 1015 km in diameter – 2000 or so in Milky Way – Favorable places for star formation (and, therefore, perhaps planetary f ...
AST443_1
... sidereal day = 24 sidereal hours, or 23h56m4s Solar time. The difference is due to the angular motion of the earth around the Sun. • The sidereal time is a measured locally. • The local sideral time (LST) is RA of the zenith. • The hour angle HA of an object with right ascension RA is given by HA=LS ...
... sidereal day = 24 sidereal hours, or 23h56m4s Solar time. The difference is due to the angular motion of the earth around the Sun. • The sidereal time is a measured locally. • The local sideral time (LST) is RA of the zenith. • The hour angle HA of an object with right ascension RA is given by HA=LS ...
Fine structure of the interplanetary shocks observed by BMSW
... There was a sharp increase of all solar wind parameters at the time of shock passage. Solar wind speed rose up on 35-40 km/s. The temperature of protons increased by 2 times after the passage of the wave. The ion concentration also increased by 2 times. Angle θBn was about 26º, according to that the ...
... There was a sharp increase of all solar wind parameters at the time of shock passage. Solar wind speed rose up on 35-40 km/s. The temperature of protons increased by 2 times after the passage of the wave. The ion concentration also increased by 2 times. Angle θBn was about 26º, according to that the ...
Solar-cycle variation of low density solar wind during
... core of CMEs observed by coronagraphs. 3) Around one quarter of low density regions occur in corotating high-speed streams. This association is not unexpected since in general faster solar wind speeds have lower densities. 4) The May 10, 1999 low density region is unusual in that it is not clearly a ...
... core of CMEs observed by coronagraphs. 3) Around one quarter of low density regions occur in corotating high-speed streams. This association is not unexpected since in general faster solar wind speeds have lower densities. 4) The May 10, 1999 low density region is unusual in that it is not clearly a ...
Enormous Eruption of 2.2 X-class Solar Flares on 10th June 2014
... mechanism for solar flares, compared with the shortcomings of the other two mechanisms [4]. In principle the magnetic energy in the solar corona is explosively released before converted into the thermal and kinetic energy in solar flares [5,6]. The eruption could possible released a temperature of t ...
... mechanism for solar flares, compared with the shortcomings of the other two mechanisms [4]. In principle the magnetic energy in the solar corona is explosively released before converted into the thermal and kinetic energy in solar flares [5,6]. The eruption could possible released a temperature of t ...
The sun and the solar corona
... Helioseismology and the Sun’s interior How do we know about the Sun’s interior? In fact, solar (and consequently) stellar models have been established by purely theoretical considerations, based on the measured energy output (luminosity), radius and mass, using of course all the applicable laws of p ...
... Helioseismology and the Sun’s interior How do we know about the Sun’s interior? In fact, solar (and consequently) stellar models have been established by purely theoretical considerations, based on the measured energy output (luminosity), radius and mass, using of course all the applicable laws of p ...
IMAP (Interstellar MApping Probe)
... second. Measurement of the interplanetary magnetic field is required for the primary science on PATH, but an ACE/MAG equivalent (dual fluxgate magnetometer with 24 vectors per second) is acceptable. A higher cadence and/or the inclusion of a search-coil magnetometer would improve the return on the s ...
... second. Measurement of the interplanetary magnetic field is required for the primary science on PATH, but an ACE/MAG equivalent (dual fluxgate magnetometer with 24 vectors per second) is acceptable. A higher cadence and/or the inclusion of a search-coil magnetometer would improve the return on the s ...
How did the solar system form? (reading
... several decades, scientists have thought that the Solar System formed as a result of a shock wave from an exploding star—a supernova—that triggered the collapse of a dense, dusty gas cloud, which then contracted to form the Sun and the planets. But detailed models of this formation process have only ...
... several decades, scientists have thought that the Solar System formed as a result of a shock wave from an exploding star—a supernova—that triggered the collapse of a dense, dusty gas cloud, which then contracted to form the Sun and the planets. But detailed models of this formation process have only ...
681_1.pdf
... and azimuthal angles; the plasma proton temperature, density and speed; and two-hour averages of the ratio Fe≥16+/Fetot, and the mean Fe charge state. In the Tp panel, the second trace indicates the "expected temperature" for normally-expanding solar wind (Tex), which is correlated with the solar wi ...
... and azimuthal angles; the plasma proton temperature, density and speed; and two-hour averages of the ratio Fe≥16+/Fetot, and the mean Fe charge state. In the Tp panel, the second trace indicates the "expected temperature" for normally-expanding solar wind (Tex), which is correlated with the solar wi ...
JOINT DISCUSSION mirror which reflects the light of the primary
... emission of hydrogen. Furthermore, this radiation appears to be of solar origin. The flux from outside the atmosphere is scattered by atomic hydrogen in space; the flux from below the rocket is scattered a second time by hydrogen in our atmosphere. The observed albedo was about 42 %. The flux of Lym ...
... emission of hydrogen. Furthermore, this radiation appears to be of solar origin. The flux from outside the atmosphere is scattered by atomic hydrogen in space; the flux from below the rocket is scattered a second time by hydrogen in our atmosphere. The observed albedo was about 42 %. The flux of Lym ...
Itinerary As Printable PDF
... become artists of understanding her. Various lines for further research will be outlined. ...
... become artists of understanding her. Various lines for further research will be outlined. ...
106_1.pdf
... particle event to solar X-ray events and set limits on the propagation length of the ions along the magnetic field lines. ...
... particle event to solar X-ray events and set limits on the propagation length of the ions along the magnetic field lines. ...
Bulletin of the American Meteorological Society
... until it is greater than the local plasma pressure, and the magnetic flux ropes expand and become buoyant (Fan, 2008) and rise through the convection zone until they break through the visible surface of the Sun, the photosphere, to be viewed as sunspots (Fig. 6). Why does a sunspot appear dark? The ...
... until it is greater than the local plasma pressure, and the magnetic flux ropes expand and become buoyant (Fan, 2008) and rise through the convection zone until they break through the visible surface of the Sun, the photosphere, to be viewed as sunspots (Fig. 6). Why does a sunspot appear dark? The ...
1. Introduction - The National Academies of Sciences, Engineering
... observations have gained in importance, but ground-based observations are still critical, not only to determine the forcing of the coronal fields by photospheric motions, but also for the measurement of the coronal magnetic field strength itself. This is important for developing and testing models ...
... observations have gained in importance, but ground-based observations are still critical, not only to determine the forcing of the coronal fields by photospheric motions, but also for the measurement of the coronal magnetic field strength itself. This is important for developing and testing models ...
Solar phenomena
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots.These phenomena are generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations.The sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather. A major weather component is the solar wind, a stream of plasma released from the Sun's upper atmosphere. It is responsible for the aurora, natural light displays in the sky in the Arctic and Antarctic. Space weather disturbances can cause solar storms on Earth, disrupting communications, as well as geomagnetic storms in Earth's magnetosphere and sudden ionospheric disturbances in the ionosphere. Variations in solar intensity also affect Earth's climate. These variations can explain events such as ice ages and the Great Oxygenation Event, while the Sun's future expansion into a red giant will likely end life on Earth.Solar activity and related events have been recorded since the 8th century BCE. Babylonians inscribed and possibly predicted solar eclipses, while the earliest extant report of sunspots dates back to the Chinese Book of Changes, c. 800 BCE. The first extant description of the solar corona was in 968, while the earliest sunspot drawing was in 1128 and a solar prominence was described in 1185 in the Russian Chronicle of Novgorod. The invention of the telescope allowed major advances in understanding, allowing the first detailed observations in the 1600s. Solar spectroscopy began in the 1800s, from which properties of the solar atmosphere could be determined, while the creation of daguerreotypy led to the first solar photographs on 2 April 1845. Photography assisted in the study of solar prominences, granulation and spectroscopy. Early in the 20th century, interest in astrophysics surged in America. A number of new observatories were built with solar telescopes around the world. The 1931 invention of the coronagraph allowed the corona to be studied in full daylight.