IRIS observations of the solar transition region
... a cadence of 54 s and is an example of a fairly longlived “nest” of loops that remains active during the entire 40-min span that the observations lasted. Movies S1, S2, and S3 show these nests to be composed of many loops with more or less cospatial footpoints that light up and darken episodically. ...
... a cadence of 54 s and is an example of a fairly longlived “nest” of loops that remains active during the entire 40-min span that the observations lasted. Movies S1, S2, and S3 show these nests to be composed of many loops with more or less cospatial footpoints that light up and darken episodically. ...
Estimation of the Sun`s rotation through the tracking of Sunspots
... First is the core; the core of the sun is where fusion takes place. This is where hydrogen is turned into helium and creates a temperature of around 15 million kelvin. This is where the light and heat we see is created. Next we have the radiation zone and the convection zone. The radiation zone is w ...
... First is the core; the core of the sun is where fusion takes place. This is where hydrogen is turned into helium and creates a temperature of around 15 million kelvin. This is where the light and heat we see is created. Next we have the radiation zone and the convection zone. The radiation zone is w ...
2003 Venkatakrishnan and Ravindra Relation between CME speed
... projected speed of halo CME. The following physical conclusions can be drawn from the study. Although emerging flux in the core of an AR may be responsible for the occurrence of a CME [Nitta and Hudson, 2001], the maximum kinetic energy released in the CME seems to be well related to the total magne ...
... projected speed of halo CME. The following physical conclusions can be drawn from the study. Although emerging flux in the core of an AR may be responsible for the occurrence of a CME [Nitta and Hudson, 2001], the maximum kinetic energy released in the CME seems to be well related to the total magne ...
From the Sun`s atmosphere to the Earth`s atmosphere
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
S.V. Berdyugina, I.G. Usoskin, Preferred Longitudes in Sunspot
... have been found to migrate in longitude as a rigid structure, seemingly due to the star’s differential rotation. This suggests that solar active longitudes, if they exist, may also follow the surface differential rotation, and the assumption on their even rotation made by previous investigators is pro ...
... have been found to migrate in longitude as a rigid structure, seemingly due to the star’s differential rotation. This suggests that solar active longitudes, if they exist, may also follow the surface differential rotation, and the assumption on their even rotation made by previous investigators is pro ...
Relationship between solar wind dynamic pressure and amplitude
... currents are small there because the ionospheric conductivities are very low in the nighttime. In the dayside, the ionospheric current of polar origin flows eastward producing a positive H-component, but it is reduced by a negative (southward) field of the FACs and the second peak appears in the ea ...
... currents are small there because the ionospheric conductivities are very low in the nighttime. In the dayside, the ionospheric current of polar origin flows eastward producing a positive H-component, but it is reduced by a negative (southward) field of the FACs and the second peak appears in the ea ...
Dissipation and heating in solar wind turbulence: from the macro to
... The physics of interplanetary space plasmas represents an archetypal non-equilibrium collective phenomenon; interdisciplinary in scope, it brings together several branches of physics from plasma physics and statistical mechanics to signal processing and high-performance computing. Plasmas exhibit di ...
... The physics of interplanetary space plasmas represents an archetypal non-equilibrium collective phenomenon; interdisciplinary in scope, it brings together several branches of physics from plasma physics and statistical mechanics to signal processing and high-performance computing. Plasmas exhibit di ...
Chapter V Conclusions Radioactive isotopes
... semi-empirical approach is best Suited for this purpose. Accurate measurement of radioisotope activity coupled with information on shapes, sizes and shielding depths in meteorite bodies provides the starting point for such an approach. The main results and conclusions arrived from the work on these ...
... semi-empirical approach is best Suited for this purpose. Accurate measurement of radioisotope activity coupled with information on shapes, sizes and shielding depths in meteorite bodies provides the starting point for such an approach. The main results and conclusions arrived from the work on these ...
8 The Sun - Journigan-wiki
... The earliest astronomers thought that the Sun was fueled by what? And would last how long? Who was the first dude to think that the Sun was power by subatomic energy? Who was the first dude to confirm it? What did Einstein have to do with all this? ...
... The earliest astronomers thought that the Sun was fueled by what? And would last how long? Who was the first dude to think that the Sun was power by subatomic energy? Who was the first dude to confirm it? What did Einstein have to do with all this? ...
The Sunspots - Scientific Research Publishing
... some regions of the photosphere, and their relationship with the appearance, properties and life time of the Sunspots. A large amount of observational data has been accumulated of the subject [1]; in particular, it is well known that the presence of Sunspots on the solar disk is related to a substan ...
... some regions of the photosphere, and their relationship with the appearance, properties and life time of the Sunspots. A large amount of observational data has been accumulated of the subject [1]; in particular, it is well known that the presence of Sunspots on the solar disk is related to a substan ...
Lecture 2: Theory - Laboratory for Atmospheric and Space Physics
... Alfvén waves with frequencies > 10 Hz have not yet been observed in the corona or solar wind, but ideas for their origin abound . . . . (1) Base generation by, e.g., “microflare” reconnection in the lanes that border convection cells (e.g., Axford & McKenzie 1997). Problem: “minor” ions consume base ...
... Alfvén waves with frequencies > 10 Hz have not yet been observed in the corona or solar wind, but ideas for their origin abound . . . . (1) Base generation by, e.g., “microflare” reconnection in the lanes that border convection cells (e.g., Axford & McKenzie 1997). Problem: “minor” ions consume base ...
Naming the 2008-2009 Minimum and Responding to Temperature Declines
... not flying, not boating, different clothes possibilities, travel changes would help us understand life. Think about the foods you eat now. How would you change your diet? How you would you respond to a frozen river or ocean and how would a frozen ocean affect the Earth? Such questions are just raise ...
... not flying, not boating, different clothes possibilities, travel changes would help us understand life. Think about the foods you eat now. How would you change your diet? How you would you respond to a frozen river or ocean and how would a frozen ocean affect the Earth? Such questions are just raise ...
The Solar Wind Power from Magnetic Flux
... Observations of polar coronal hole flows from Ulysses’ 3rd orbit showed characteristic differences in the solar wind compared to the previous solar cycle. The fast wind was slightly slower and significantly less dense, cooler, and had less mass and momentum flux than during the previous solar minimu ...
... Observations of polar coronal hole flows from Ulysses’ 3rd orbit showed characteristic differences in the solar wind compared to the previous solar cycle. The fast wind was slightly slower and significantly less dense, cooler, and had less mass and momentum flux than during the previous solar minimu ...
Stellar Spectroscopy during Exoplanet Transits
... Snapshots of emergent intensity during granular evolution on a 12,000 K white dwarf (left) and a 3,800 K red giant. Horizontal areas differ by dozen orders of magnitude: 7x7 km2 for the white dwarf, and 23x23 RSun2 for the giant. (H.-G. Ludwi,g, Heidelberg) ...
... Snapshots of emergent intensity during granular evolution on a 12,000 K white dwarf (left) and a 3,800 K red giant. Horizontal areas differ by dozen orders of magnitude: 7x7 km2 for the white dwarf, and 23x23 RSun2 for the giant. (H.-G. Ludwi,g, Heidelberg) ...
C-14 is used to date
... With increased solar activity the magnetic field of the sun intensifies, which shields the earth from cosmic rays from the sun. So less C-14 is produced when the sun has a high sunspot population. ...
... With increased solar activity the magnetic field of the sun intensifies, which shields the earth from cosmic rays from the sun. So less C-14 is produced when the sun has a high sunspot population. ...
THE LUYINOSITY VARIABILITY OF SOLAR
... emission and rotation rate are both proportional to the inverse square root of stellar age for stars of similar mass: [Skumanich, 1972]) remains a simple and useful rule for lower main-sequence stars throughout much of the age range considered here, despite the fact that it fails for very young star ...
... emission and rotation rate are both proportional to the inverse square root of stellar age for stars of similar mass: [Skumanich, 1972]) remains a simple and useful rule for lower main-sequence stars throughout much of the age range considered here, despite the fact that it fails for very young star ...
Midterm Presentation
... • Verify the computation of shading and blocking for 8 mirrors done by the previous capstone team. • Calculate shading and blocking for 24 mirrors. • Use Java-3D software to show the graphical representation of levels of shading and blocking. • Use slit mirror design to maximize the efficiency of he ...
... • Verify the computation of shading and blocking for 8 mirrors done by the previous capstone team. • Calculate shading and blocking for 24 mirrors. • Use Java-3D software to show the graphical representation of levels of shading and blocking. • Use slit mirror design to maximize the efficiency of he ...
Turbulent Origins of the Solar Wind
... Why is the fast/slow wind fast/slow? • Several ideas exist; one powerful one relates the spatial dependence of the heating to the location of the Parker critical point; this determines how the “available” heating affects the plasma (e.g., Leer & Holzer 1980): SUPERSONIC coronal heating: subsonic re ...
... Why is the fast/slow wind fast/slow? • Several ideas exist; one powerful one relates the spatial dependence of the heating to the location of the Parker critical point; this determines how the “available” heating affects the plasma (e.g., Leer & Holzer 1980): SUPERSONIC coronal heating: subsonic re ...
The role of the sun in climate forcing
... activity regime during the solar rotation. So, the TSI is a mixture of all these temporal and spatial phenomena and it is di$cult to attribute the observed irradiance variations to a single feature in the photosphere. The observed irradiance variability is essentially the response of the outer solar ...
... activity regime during the solar rotation. So, the TSI is a mixture of all these temporal and spatial phenomena and it is di$cult to attribute the observed irradiance variations to a single feature in the photosphere. The observed irradiance variability is essentially the response of the outer solar ...
Turbulent Origins of the Solar Wind
... Why is the fast/slow wind fast/slow? • Several ideas exist; one powerful one relates the spatial dependence of the heating to the location of the Parker critical point; this determines how the “available” heating affects the plasma (e.g., Leer & Holzer 1980): SUPERSONIC coronal heating: subsonic re ...
... Why is the fast/slow wind fast/slow? • Several ideas exist; one powerful one relates the spatial dependence of the heating to the location of the Parker critical point; this determines how the “available” heating affects the plasma (e.g., Leer & Holzer 1980): SUPERSONIC coronal heating: subsonic re ...
Generation of highly energetic electrons at
... released and transferred into a local heating of the coronal plasma, mass motions (e.g. jets), enhanced emission of electromagnetic radiation (from the radio up to the γray range), and energetic particles (e.g. electrons, protons, and heavy ions). The electrons play an important role, since they car ...
... released and transferred into a local heating of the coronal plasma, mass motions (e.g. jets), enhanced emission of electromagnetic radiation (from the radio up to the γray range), and energetic particles (e.g. electrons, protons, and heavy ions). The electrons play an important role, since they car ...
Studies on post-flare loop prominence of 1981 April 27
... (i) We could not find any He filaments or any filament-like structure parallel to Htt= 0 line before the flare. (ii) The magnetic structure of the active region where the 1981 April 27 flare occurred is not favourable for forming a magnetic system of sheared loops which bridges the H Jl = 0 line. Th ...
... (i) We could not find any He filaments or any filament-like structure parallel to Htt= 0 line before the flare. (ii) The magnetic structure of the active region where the 1981 April 27 flare occurred is not favourable for forming a magnetic system of sheared loops which bridges the H Jl = 0 line. Th ...
The Sun
... Solar Neutrino Puzzle Unreactive and Large mean free path !!! Solar neutrinos originate from the core of the Sun due to thermonuclear reactions and thus offer the possibility of probing solar interior. They are highly unreactive and even pass through the Earth undetected. Flux at Earth is of the ord ...
... Solar Neutrino Puzzle Unreactive and Large mean free path !!! Solar neutrinos originate from the core of the Sun due to thermonuclear reactions and thus offer the possibility of probing solar interior. They are highly unreactive and even pass through the Earth undetected. Flux at Earth is of the ord ...
Fulltext PDF
... over peninsular India. An important discovery, made during this eclipse by W W Campbell, an American astronomer was that the pearly white corona was strongly polarized. This observation indicated the presence of material particles in the corona (to scatter the photospheric light). Today we know that ...
... over peninsular India. An important discovery, made during this eclipse by W W Campbell, an American astronomer was that the pearly white corona was strongly polarized. This observation indicated the presence of material particles in the corona (to scatter the photospheric light). Today we know that ...
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.