Jack Eddy`s Study of the Maunder Minimum Inspires a Long Series
... • Maunder Minimum (MM) period in late 1600s has lower solar activity – How much of the colder temperature (-0.4 K) during MM was driven by solar irradiance change? • Even if cycle minimum did not change during MM, Georg Feulner’s climate model (GRL, 2011) predicts a colder period because of cycle ...
... • Maunder Minimum (MM) period in late 1600s has lower solar activity – How much of the colder temperature (-0.4 K) during MM was driven by solar irradiance change? • Even if cycle minimum did not change during MM, Georg Feulner’s climate model (GRL, 2011) predicts a colder period because of cycle ...
A diffusive description of the focused transport of solar energetic
... scale that characterizes the change in B0 is large compared to the spatial dimension of the particles’ gyration motion. In this case it can be assumed that B0 is constant for a single gyration, and the first adiabatic invariant is conserved. For a particle moving in a diverging magnetic field, this ...
... scale that characterizes the change in B0 is large compared to the spatial dimension of the particles’ gyration motion. In this case it can be assumed that B0 is constant for a single gyration, and the first adiabatic invariant is conserved. For a particle moving in a diverging magnetic field, this ...
Doubly Ionized Carbon Observed in the Plasma Tail of Comet Kudo
... give QH ⫽ 1.1 ⫻ 1030 s⫺1 at the time of the first crossing, increasing to 5.3 ⫻ 1030 s⫺1 by the last crossing. These numbers correspond to water outgassing rates of 5.5 ⫻ 1029 s⫺1 to 2.65 ⫻ 1030 s⫺1. The model can be modified to use the radiance of the H I Ly  102.6-nm line instead, allowing us to ...
... give QH ⫽ 1.1 ⫻ 1030 s⫺1 at the time of the first crossing, increasing to 5.3 ⫻ 1030 s⫺1 by the last crossing. These numbers correspond to water outgassing rates of 5.5 ⫻ 1029 s⫺1 to 2.65 ⫻ 1030 s⫺1. The model can be modified to use the radiance of the H I Ly  102.6-nm line instead, allowing us to ...
Ice Core Records - Chandra X
... unique solar proton events. These peaks are several standard deviations above the mean. It is likely that these anomalies result from the primary production of nitrate (NO3-) in the atmosphere – therefore there has to be an enhanced supply of nitrate in the stratosphere. In the GSIP2-H core segment ...
... unique solar proton events. These peaks are several standard deviations above the mean. It is likely that these anomalies result from the primary production of nitrate (NO3-) in the atmosphere – therefore there has to be an enhanced supply of nitrate in the stratosphere. In the GSIP2-H core segment ...
Scientific Analysis within SEPServer
... propagation theories through numerical simulations and comparisons with the in-situ measurements. SEP events originate by either solar flares or coronal mass ejections (CMEs) (Reames, 1999) and are frequently (but roughly) categorized as gradual or impulsive. The production of SEP events related to ...
... propagation theories through numerical simulations and comparisons with the in-situ measurements. SEP events originate by either solar flares or coronal mass ejections (CMEs) (Reames, 1999) and are frequently (but roughly) categorized as gradual or impulsive. The production of SEP events related to ...
Observation of the Bastille day flare on 2000 July 14
... arcade, the distance between ribbons would become wider and wider. Why the magnetic reconnection could explain the problem of particles accelerating? According to Faraday’s Law, the magnetic arcade which has changing magnetic flux would form an electric current called reconnection current sheet tha ...
... arcade, the distance between ribbons would become wider and wider. Why the magnetic reconnection could explain the problem of particles accelerating? According to Faraday’s Law, the magnetic arcade which has changing magnetic flux would form an electric current called reconnection current sheet tha ...
Electron and Ion Dynamics of the Solar Wind Interaction with a
... are critical to decipher the physics of gas release processes in space. The latter result in mass-loaded plasmas [9,10], which more than three decades after the Active Magnetospheric Particle Tracer Explorers (AMPTE) space release experiments [11] are still not fully understood. First observed in 19 ...
... are critical to decipher the physics of gas release processes in space. The latter result in mass-loaded plasmas [9,10], which more than three decades after the Active Magnetospheric Particle Tracer Explorers (AMPTE) space release experiments [11] are still not fully understood. First observed in 19 ...
Neutrino Physics M. SPURIO University of Bologna and INFN
... Once the core of the star becomes constituted primarily of iron, further compression of the core does not ignite nuclear fusion and the star is unable to thermodynamically support its outer envelope. As the surrounding matter falls inward under gravity, the temperature of the core rises and iron ...
... Once the core of the star becomes constituted primarily of iron, further compression of the core does not ignite nuclear fusion and the star is unable to thermodynamically support its outer envelope. As the surrounding matter falls inward under gravity, the temperature of the core rises and iron ...
PDF - Isaac Scientific Publishing
... Abstract. To get accurate knowledge about the longitudinal motion of the Moon we must use the oldest preserved interpretable depictions and texts from the ancient cultures. 33 ancient total or almost total solar eclipses, back to 3653 BC, have been used to determine the lunar sidereal secular accele ...
... Abstract. To get accurate knowledge about the longitudinal motion of the Moon we must use the oldest preserved interpretable depictions and texts from the ancient cultures. 33 ancient total or almost total solar eclipses, back to 3653 BC, have been used to determine the lunar sidereal secular accele ...
Dynamic Martian magnetosphere: Transient - HAL
... suited to investigate this particular region and needs to be completed with a ionospheric model taking into account the main chemical reactions and the electrical conductivities. 3.3. Response of the Magnetic Lobes [9] In response to the draped field lines around the obstacle, a bipolar magnetic tai ...
... suited to investigate this particular region and needs to be completed with a ionospheric model taking into account the main chemical reactions and the electrical conductivities. 3.3. Response of the Magnetic Lobes [9] In response to the draped field lines around the obstacle, a bipolar magnetic tai ...
Session 1: Structure and dynamics of the solar chromosphere
... chromosphere (cell interior, network, spicules etc.) as well as other features seen at the chromospheric level or having the properties of plasmas at chromospheric temperatures: sunspots chromosphere, plages, chromospheric flares, filaments etc. The relation of such plasmas to other atmospheric laye ...
... chromosphere (cell interior, network, spicules etc.) as well as other features seen at the chromospheric level or having the properties of plasmas at chromospheric temperatures: sunspots chromosphere, plages, chromospheric flares, filaments etc. The relation of such plasmas to other atmospheric laye ...
Lecture 13 Presupernova Models, Core Collapse and Bounce
... core collapses in a sef similar fashion. Were = 4/3 for the entire iron core, the entire core would contract homologously, but because becomes significantly less than 4/3, part of the inner core pulls away from the outer core. As the center of this inner core approaches and exceeds nuc the resi ...
... core collapses in a sef similar fashion. Were = 4/3 for the entire iron core, the entire core would contract homologously, but because becomes significantly less than 4/3, part of the inner core pulls away from the outer core. As the center of this inner core approaches and exceeds nuc the resi ...
Introduction to HI Paper
... Heliospheric Imager (HI) (Socker et al., 2000; Defise et al., 2003, Harrison et al., 2005). It is this instrument, aboard STEREO, which provides wide-angle imaging of the heliosphere in order to study ejecta in interplanetary space. HI consists of two small telescope systems mounted on the side of e ...
... Heliospheric Imager (HI) (Socker et al., 2000; Defise et al., 2003, Harrison et al., 2005). It is this instrument, aboard STEREO, which provides wide-angle imaging of the heliosphere in order to study ejecta in interplanetary space. HI consists of two small telescope systems mounted on the side of e ...
How does the solar wind blow? A simple kinetic model
... For science-fiction writers and some space engineers, the ‘wind from the Sun’ [7] is the thrust of the solar radiation pressure, which (in theory [4]) would allow solar sailing and might drive space windjammers through the inner solar system. Yet the Sun produces another kind of wind, made of partic ...
... For science-fiction writers and some space engineers, the ‘wind from the Sun’ [7] is the thrust of the solar radiation pressure, which (in theory [4]) would allow solar sailing and might drive space windjammers through the inner solar system. Yet the Sun produces another kind of wind, made of partic ...
Here - HESPERIA
... Observations with Fermi/LAT have revealed over twenty-five >100 MeV gamma-ray events on the Sun lasting from tens of minutes to several hours. All are associated with flares and all but one with fast CMEs. The gamma-ray emission is most probably from decay of pions produced by high-energy proton and ...
... Observations with Fermi/LAT have revealed over twenty-five >100 MeV gamma-ray events on the Sun lasting from tens of minutes to several hours. All are associated with flares and all but one with fast CMEs. The gamma-ray emission is most probably from decay of pions produced by high-energy proton and ...
heavenly bodies
... Because the relative orbital speed of the comet and the solar wind is supersonic, a bow shock is formed upstream of the comet in the flow direction of the solar wind. In this bow shock, large concentrations of cometary ions (called "pick-up ions") congregate and act to "load" the solar magnetic fie ...
... Because the relative orbital speed of the comet and the solar wind is supersonic, a bow shock is formed upstream of the comet in the flow direction of the solar wind. In this bow shock, large concentrations of cometary ions (called "pick-up ions") congregate and act to "load" the solar magnetic fie ...
here - The Planetary Chemistry Laboratory
... the photosphere all stable elements up to atomic number 83 (Bi) plus radioactive Th and U ~30 – 35 elements well determined in photosphere Determined in photosphere with larger uncertainties: ...
... the photosphere all stable elements up to atomic number 83 (Bi) plus radioactive Th and U ~30 – 35 elements well determined in photosphere Determined in photosphere with larger uncertainties: ...
Diffusion of Open Magnetic Flux and Its Consequences
... It is important to treat the open flux and the solar wind as a coupled problem. Open flux can be considered to be open only if there is a flo w of solar wind along it that is capable of carrying the open flux out into th e ...
... It is important to treat the open flux and the solar wind as a coupled problem. Open flux can be considered to be open only if there is a flo w of solar wind along it that is capable of carrying the open flux out into th e ...
BDW Lesson 1g - Ohio Academic Standards
... create? [Crustal deformation, spin axis shift, catastrophic event] 2) Was there a Planet X [14] [15] between Mars and Jupiter as predicted by the Titus Bode law [Possible, this would fit law]. The Asteroid belts now inhabit this region of the Solar System. What effects might Asteroid collision with ...
... create? [Crustal deformation, spin axis shift, catastrophic event] 2) Was there a Planet X [14] [15] between Mars and Jupiter as predicted by the Titus Bode law [Possible, this would fit law]. The Asteroid belts now inhabit this region of the Solar System. What effects might Asteroid collision with ...
Solar Irradiance Reference Spectra (SIRS) for the 2008 Whole
... the prototype EUV Variability Experiment (EVE) developed for the future Solar Dynamics Observatory (SDO) mission. Along with using these observations, which are the most accurate to date, another goal for the WHI SIRS is to provide higher spectral resolution. The full spectral range from 0.1 to 2400 ...
... the prototype EUV Variability Experiment (EVE) developed for the future Solar Dynamics Observatory (SDO) mission. Along with using these observations, which are the most accurate to date, another goal for the WHI SIRS is to provide higher spectral resolution. The full spectral range from 0.1 to 2400 ...
On the origin of the fast solar wind in polar coronal funnels
... what the plasma properties in the funnel are. Thereby the flow close to the surface must be in agreement with SUMER/SOHO observations in Neviii of up flow (blue shifts). Also the Ulysses mass flux, which puts when mapped back to the funnel bottom a constraint on the flow, and more importantly requir ...
... what the plasma properties in the funnel are. Thereby the flow close to the surface must be in agreement with SUMER/SOHO observations in Neviii of up flow (blue shifts). Also the Ulysses mass flux, which puts when mapped back to the funnel bottom a constraint on the flow, and more importantly requir ...
Spots on Ap Stars
... • 10-15% of late B-early F stars have magnetic fields (Sr-CrEu stars, Si stars) • Oblique rotator model – dipole field inclined to rotation axis (and also decentered) • High Teff and stable atmospheres • Radiative and gravitational forces push atoms up or down ...
... • 10-15% of late B-early F stars have magnetic fields (Sr-CrEu stars, Si stars) • Oblique rotator model – dipole field inclined to rotation axis (and also decentered) • High Teff and stable atmospheres • Radiative and gravitational forces push atoms up or down ...
Measuring the angular solar diameter using two pinholes
... where d m is the diameter of the image on the screen, d p is the diameter of the pinhole, and f is the focal length. The latter is the distance between the center of the image on the screen S and the center of the pinhole, mounted on a mask M parallel to the screen 共see Fig. 1兲. The mean angular sol ...
... where d m is the diameter of the image on the screen, d p is the diameter of the pinhole, and f is the focal length. The latter is the distance between the center of the image on the screen S and the center of the pinhole, mounted on a mask M parallel to the screen 共see Fig. 1兲. The mean angular sol ...
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.