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... Correlations between variations in Solar EUV and soft X-‐ray irradiance and photoelectron energy spectra observed on Mars and Earth ...
... Correlations between variations in Solar EUV and soft X-‐ray irradiance and photoelectron energy spectra observed on Mars and Earth ...
Mars Express - The Scientific Investigations: ASPERA-3
... but a large fraction is emitted via charge exchange when hot plasma, of solar wind and planetary wind origin, interacts with the upper atmosphere. In this chapter we briefly review three ENA phenomena related to Mars – ENA albedo, ENA jets and ENA occultation. We also discuss another, yet to be expl ...
... but a large fraction is emitted via charge exchange when hot plasma, of solar wind and planetary wind origin, interacts with the upper atmosphere. In this chapter we briefly review three ENA phenomena related to Mars – ENA albedo, ENA jets and ENA occultation. We also discuss another, yet to be expl ...
Simultaneous observation of the electron acceleration and ion deceleration
... with higher energy than the solar wind protons were ions pick-up accelerated by the solar wind convection electric field (Saito et al., 2008b). The intense ions observed between 0815 UT and 0835 UT (indicated by a blue box) were the ions reflected by magnetic anomalies on the lunar surface. When mag ...
... with higher energy than the solar wind protons were ions pick-up accelerated by the solar wind convection electric field (Saito et al., 2008b). The intense ions observed between 0815 UT and 0835 UT (indicated by a blue box) were the ions reflected by magnetic anomalies on the lunar surface. When mag ...
Numerical models of sunspot formation and fine structure
... Sunspots are central to our understanding of solar (and stellar) magnetism in many respects. On the large scale, they link the magnetic field observable in the photosphere to the dynamo processes operating in the solar interior. Properly interpreting the constraints that sunspots impose on the dynamo ...
... Sunspots are central to our understanding of solar (and stellar) magnetism in many respects. On the large scale, they link the magnetic field observable in the photosphere to the dynamo processes operating in the solar interior. Properly interpreting the constraints that sunspots impose on the dynamo ...
release history and transport parameters of relativistic solar
... The two pioneering Helios spacecraft explored the inner heliosphere (from 0.29 to 0.98 AU) during solar cycle 21 and captured several SEP events during their fast perihelion passages. In this work, we re-visit a sequence of four consecutive relativistic electron events observed by Helios-1 at 0.31 A ...
... The two pioneering Helios spacecraft explored the inner heliosphere (from 0.29 to 0.98 AU) during solar cycle 21 and captured several SEP events during their fast perihelion passages. In this work, we re-visit a sequence of four consecutive relativistic electron events observed by Helios-1 at 0.31 A ...
Observations and analysis of phase scintillation of spacecraft signal
... (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its speed. Fast winds are seen above coronal holes and can las ...
... (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its speed. Fast winds are seen above coronal holes and can las ...
- 1 - Ulysses Observations of Solar Energetic Particles From the July
... Energetic particles from ~1 MeV to a few GeV observed in the heliospace may come from various acceleration sources. They may be galactic cosmic rays, anomalous cosmic rays accelerated by the termination shock, energetic particles accelerated by interplanetary shock, or solar energetic particles acce ...
... Energetic particles from ~1 MeV to a few GeV observed in the heliospace may come from various acceleration sources. They may be galactic cosmic rays, anomalous cosmic rays accelerated by the termination shock, energetic particles accelerated by interplanetary shock, or solar energetic particles acce ...
Cosmic Rays near Proxima Centauri b
... the Sun and a mass of about 12 per cent of the mass of the Sun (GJ 551; dM5.5e) (see Anglada-Escude et al. (2016)). Anglada-Escude et al. (2016) reported the presence of a small planet with a minimum mass of about 1.3 Earth masses orbiting Proxima with a period of approximately 11.2 days at a semi-m ...
... the Sun and a mass of about 12 per cent of the mass of the Sun (GJ 551; dM5.5e) (see Anglada-Escude et al. (2016)). Anglada-Escude et al. (2016) reported the presence of a small planet with a minimum mass of about 1.3 Earth masses orbiting Proxima with a period of approximately 11.2 days at a semi-m ...
What is Beneath the Sunspots? Home Page ____________________________________________
... Sunspots are the dark spots seen on sun’s surface [5], they are regions where strong magnetic fields emerge from solar interior and where major eruptive events occurs [6], it was studied individually as a phenomenon with strong magnetic field [5]. Until now, sunspots are conceived as a magnetic flu ...
... Sunspots are the dark spots seen on sun’s surface [5], they are regions where strong magnetic fields emerge from solar interior and where major eruptive events occurs [6], it was studied individually as a phenomenon with strong magnetic field [5]. Until now, sunspots are conceived as a magnetic flu ...
Chapter 15--Our Sun - Geological Sciences
... the Sun has its own version of weather, in which conditions at a particular altitude differ from one region to another. Some regions of the chromosphere and corona are particularly hot and bright, while other regions are cooler and less dense. In the photosphere, sunspots are cooler than the surroun ...
... the Sun has its own version of weather, in which conditions at a particular altitude differ from one region to another. Some regions of the chromosphere and corona are particularly hot and bright, while other regions are cooler and less dense. In the photosphere, sunspots are cooler than the surroun ...
Mass transport in the heliosphere by energetic neutral atoms
... protons would thus reach, after charge exchange in the heliospheric sheath, the inner heliosphere as ENAs. Second, the slowing down of the solar wind would shift (in the velocity space) the distribution of the solar wind pick up protons, and some of these protons would reach, after charge exchange, ...
... protons would thus reach, after charge exchange in the heliospheric sheath, the inner heliosphere as ENAs. Second, the slowing down of the solar wind would shift (in the velocity space) the distribution of the solar wind pick up protons, and some of these protons would reach, after charge exchange, ...
Who’s Afraid of a Stellar Superflare? Rachel Osten GSFC
... superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
... superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
ASPERA-3: Analyser of Space Plasmas and
... effects of such ENA precipitation using Monte Carlo simulations and estimated that, under typical solar wind conditions, the precipitating hydrogen atoms increase the ionisation rate by about 1% in comparison with ionisation rates owing to extreme UV radiation. This effect is comparable to, or even ...
... effects of such ENA precipitation using Monte Carlo simulations and estimated that, under typical solar wind conditions, the precipitating hydrogen atoms increase the ionisation rate by about 1% in comparison with ionisation rates owing to extreme UV radiation. This effect is comparable to, or even ...
chapter5 - Homework Market
... from the sun and other stars are all produced by moving electrons. • As you know, an atom has a massive compact nucleus containing positively charged protons. • These are usually accompanied by electrically neutral neutrons. • The nucleus is embedded in a large cloud of relatively low-mass, negative ...
... from the sun and other stars are all produced by moving electrons. • As you know, an atom has a massive compact nucleus containing positively charged protons. • These are usually accompanied by electrically neutral neutrons. • The nucleus is embedded in a large cloud of relatively low-mass, negative ...
the amplitude of solar oscillations using stellar techniques
... Hydrus, Pavo, Serpens, Indus) — stars: oscillations Online material: color figures 1. INTRODUCTION ...
... Hydrus, Pavo, Serpens, Indus) — stars: oscillations Online material: color figures 1. INTRODUCTION ...
Dating the Earliest Solids in our Solar System
... It appears that 26Al can be used as a clock to measure small time differences, allowing us to understand more about the formation of the first solids in the solar system. Preliminary Al-Mg results for chondrules from the CR and CV chondrites by K. K. Marhas (Physical Research Lab, India) and colleag ...
... It appears that 26Al can be used as a clock to measure small time differences, allowing us to understand more about the formation of the first solids in the solar system. Preliminary Al-Mg results for chondrules from the CR and CV chondrites by K. K. Marhas (Physical Research Lab, India) and colleag ...
2 Solar magnetic fields. - High Altitude Observatory
... Fig. 2.3. Distributions of flares for the Sun in comparison with stars, modified from Shibata et al. (2013) to include the “Carrington Event”. The solid histogram shows the frequency distribution of superflares on G V -type stars with rotational period > 10 d and effective temperatures of 5600–6000 K ...
... Fig. 2.3. Distributions of flares for the Sun in comparison with stars, modified from Shibata et al. (2013) to include the “Carrington Event”. The solid histogram shows the frequency distribution of superflares on G V -type stars with rotational period > 10 d and effective temperatures of 5600–6000 K ...
Plasma waves above the ion cyclotron frequency in the solar wind: a
... The solar wind energy spectrum shows that the energy is distributed over a broad range of frequencies (Fig. 2). Three zones are usually distinguished following the exponent α of the power law that characterizes each of them: the very low energy regime with α≈−1, the inertial region (roughly 10−4 Hz< ...
... The solar wind energy spectrum shows that the energy is distributed over a broad range of frequencies (Fig. 2). Three zones are usually distinguished following the exponent α of the power law that characterizes each of them: the very low energy regime with α≈−1, the inertial region (roughly 10−4 Hz< ...
CEA - The Sun
... loss of energy at the surface and allows the Sun to burn sustainably; contraction causes an increase in heating providing the energy to remain in balance from its gravitational capital. In reality, these two phenomena are linked: since the nuclear resources are limited, gravitational contraction of ...
... loss of energy at the surface and allows the Sun to burn sustainably; contraction causes an increase in heating providing the energy to remain in balance from its gravitational capital. In reality, these two phenomena are linked: since the nuclear resources are limited, gravitational contraction of ...
icso2000_picard
... large CCD) is confirmed and performances in the range of ± 2 mas on the absolute solar Diameter measure is foreseen. Relative measures to a significant fraction of a mas are probably possible. Despite the excellent properties of SiC, the heavy thermal load generated by Solar observing requires a car ...
... large CCD) is confirmed and performances in the range of ± 2 mas on the absolute solar Diameter measure is foreseen. Relative measures to a significant fraction of a mas are probably possible. Despite the excellent properties of SiC, the heavy thermal load generated by Solar observing requires a car ...
Skywave Excitement - Lake Area Radio Klub
... When they are sent into the ionosphere, radio waves with frequencies below the Maximum Usable Frequency (MUF) and above the Lowest Usable Frequency (LUF) are bent back to the Earth. (G3B05) A reliable way to determine if the Maximum Usable Frequency (MUF) is high enough to support skip propagati ...
... When they are sent into the ionosphere, radio waves with frequencies below the Maximum Usable Frequency (MUF) and above the Lowest Usable Frequency (LUF) are bent back to the Earth. (G3B05) A reliable way to determine if the Maximum Usable Frequency (MUF) is high enough to support skip propagati ...
Solar chromospheric flares: energy release, transport and radiation
... footpoint emission (Sakao et al. 1996; Krucker & Lin 2002), and since it is clear from non-thermal HXR emission - generated by the electron-proton bremsstrahlung mechanism - that there are copious numbers of electrons present in the chromosphere, which is also strongly heated, a beam of high energy ...
... footpoint emission (Sakao et al. 1996; Krucker & Lin 2002), and since it is clear from non-thermal HXR emission - generated by the electron-proton bremsstrahlung mechanism - that there are copious numbers of electrons present in the chromosphere, which is also strongly heated, a beam of high energy ...
PPT
... balanced and solve (poloidal) field aligned flow. • If we consider more realistic situation in 2D, we need to solve additional equation, so-called Grad-Shafranov equation (trans-field equation) which describing force balance perpendicular to poloidal field line coupling with wind equations. • In gen ...
... balanced and solve (poloidal) field aligned flow. • If we consider more realistic situation in 2D, we need to solve additional equation, so-called Grad-Shafranov equation (trans-field equation) which describing force balance perpendicular to poloidal field line coupling with wind equations. • In gen ...
Upper ionosphere of Mars is not axially symmetrical
... a function of the altitude (third and fourth panels) clearly show this asymmetry. Similar asymmetry between the inbound and outbound crossings is seen in Fig. 4 which shows the altitude profiles of cold oxygen ions measured by IMA-ASPERA-3 on several orbits sampling the same solar zenith angles. The ...
... a function of the altitude (third and fourth panels) clearly show this asymmetry. Similar asymmetry between the inbound and outbound crossings is seen in Fig. 4 which shows the altitude profiles of cold oxygen ions measured by IMA-ASPERA-3 on several orbits sampling the same solar zenith angles. The ...
Protecting planets from their stars
... where magnetic field lines are open (coronal holes) and the slow solar wind emerges above the low-latitude active regions (latitudes of up to 30–35° around the equator). In contrast, during periods of maximum activity, the topology of the field becomes more complicated, affecting the solar wind: by ...
... where magnetic field lines are open (coronal holes) and the slow solar wind emerges above the low-latitude active regions (latitudes of up to 30–35° around the equator). In contrast, during periods of maximum activity, the topology of the field becomes more complicated, affecting the solar wind: by ...
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.