A straightforward estimation of the maximum sunspot number for
... Simon and Legrand (1987) studying cycles 11 to 21 found that at the peak of the quiet days the heliosheet has its maximum thickness; this occurs at the end of the dipole phase when the solar dipole is weakest, near solar minimum. It has been also shown that the evolution of the poloidal ®eld is in a ...
... Simon and Legrand (1987) studying cycles 11 to 21 found that at the peak of the quiet days the heliosheet has its maximum thickness; this occurs at the end of the dipole phase when the solar dipole is weakest, near solar minimum. It has been also shown that the evolution of the poloidal ®eld is in a ...
Spin down of a stellar interior 1 Introduction Rosalind Oglethorpe
... Helioseismology has revealed a lot of information about the structure and dynamics of the solar interior, and we expect astroseismology from the Kepler probe to soon reveal similar information about other solar-type stars. The Sun and solar-type stars have two regions: a convective outer zone and a ...
... Helioseismology has revealed a lot of information about the structure and dynamics of the solar interior, and we expect astroseismology from the Kepler probe to soon reveal similar information about other solar-type stars. The Sun and solar-type stars have two regions: a convective outer zone and a ...
dark matter?
... movement is in the same direction as our solar system’s path around the galaxy, so the detected signal should increase. In December, Earth moves in the opposite direction, and scientists should detect a signal some 5 to 10 percent smaller. This signal difference helps distinguish the WIMPs from the ...
... movement is in the same direction as our solar system’s path around the galaxy, so the detected signal should increase. In December, Earth moves in the opposite direction, and scientists should detect a signal some 5 to 10 percent smaller. This signal difference helps distinguish the WIMPs from the ...
The Birth Environment of the Solar System
... giant planets is estimated to be about 20 percent (although larger fractions, perhaps up to 50 percent, remain possible). At this time, detection of planets with masses comparable to Earth is just out of reach for main-sequence stars (due to technical limitations). As a result, it is too early to as ...
... giant planets is estimated to be about 20 percent (although larger fractions, perhaps up to 50 percent, remain possible). At this time, detection of planets with masses comparable to Earth is just out of reach for main-sequence stars (due to technical limitations). As a result, it is too early to as ...
Starry Night Pro Student Exercises
... The Tool Palette is normally found floating on the left side of the screen. Clicking on the Object Selection Tool allows you to identify any object on the screen by pointing to an object and clicking the right mouse button. Use of the Constellation Tool will be explained in Exercise 2. Normally, the ...
... The Tool Palette is normally found floating on the left side of the screen. Clicking on the Object Selection Tool allows you to identify any object on the screen by pointing to an object and clicking the right mouse button. Use of the Constellation Tool will be explained in Exercise 2. Normally, the ...
SUMER/SOHO Filament Observations in Selected Lyman Lines B
... The target of SUMER on board the SOHO satellite was part of a North-South filament (S6-12, E5), close to a bright network cell (see Ha spectroheliogram from Meudon, Figure la). SUMER has been described by Wilhelm et al. (1997). SUMER was rastering a region 120 by 150 arc sec with a raster-step of 3 ...
... The target of SUMER on board the SOHO satellite was part of a North-South filament (S6-12, E5), close to a bright network cell (see Ha spectroheliogram from Meudon, Figure la). SUMER has been described by Wilhelm et al. (1997). SUMER was rastering a region 120 by 150 arc sec with a raster-step of 3 ...
dark matter effective field theories in stars
... We used a consistent and robust solar model to obtain upper limits placed by neutrino telescopes, such as IceCube and Super-Kamiokande, on the dark matter-nucleon scattering cross-section, for a general model of dark matter with a velocity dependent (p-wave) thermally averaged cross-section. In this ...
... We used a consistent and robust solar model to obtain upper limits placed by neutrino telescopes, such as IceCube and Super-Kamiokande, on the dark matter-nucleon scattering cross-section, for a general model of dark matter with a velocity dependent (p-wave) thermally averaged cross-section. In this ...
Fulltext
... It is therefore natural to ask whether there exist stable stellar configurations other than dwarfs, neutron stars, and black holes. The central density of a typical neutron star is often greater than several times the nuclear matter density P~.~. (= 2 x 10r4gm/cm3). At such high density, neutron mat ...
... It is therefore natural to ask whether there exist stable stellar configurations other than dwarfs, neutron stars, and black holes. The central density of a typical neutron star is often greater than several times the nuclear matter density P~.~. (= 2 x 10r4gm/cm3). At such high density, neutron mat ...
Circumstellar medium around rotating massive stars at solar metallicity
... The second new tool is an elaborate, object-oriented implementation of the description of time-dependent stellar boundary conditions for entire stellar systems. For the present study, it allows us to accommodate in an easy and transparent way the timedependent boundary conditions of our single star. ...
... The second new tool is an elaborate, object-oriented implementation of the description of time-dependent stellar boundary conditions for entire stellar systems. For the present study, it allows us to accommodate in an easy and transparent way the timedependent boundary conditions of our single star. ...
Investigation of mass flows in the transition region and corona in a
... set of equations being solved includes the continuity equation, the induction equation, the Navier-Stokes equation, and the energy equation with an anisotropic Spitzer heat conduction term (Spitzer 1962) and an optical thin radiative loss function (Cook et al. 1989). For the lower boundary we constr ...
... set of equations being solved includes the continuity equation, the induction equation, the Navier-Stokes equation, and the energy equation with an anisotropic Spitzer heat conduction term (Spitzer 1962) and an optical thin radiative loss function (Cook et al. 1989). For the lower boundary we constr ...
Transiting planets from WASP
... The photometric baseline models aim to represent astrophysical, instrumental, or environmental effects, which are able to produce photometric variations and can, therefore, affect the transit light curves. They are made up of different first to fourthorder polynomials with respect to time or other vari ...
... The photometric baseline models aim to represent astrophysical, instrumental, or environmental effects, which are able to produce photometric variations and can, therefore, affect the transit light curves. They are made up of different first to fourthorder polynomials with respect to time or other vari ...
1 December 2014 An Update on the Universe Professor Ian Morison
... but was renamed after the death of one of the pioneers of CMB observations, Dave Wilkinson, who sadly died of cancer whilst its data was being analysed. The WMAP spacecraft was launched on 30 June 2001 and flew to the Sun-Earth “L2 Lagrangian point”, arriving there on 1 October 2001. This lies at a ...
... but was renamed after the death of one of the pioneers of CMB observations, Dave Wilkinson, who sadly died of cancer whilst its data was being analysed. The WMAP spacecraft was launched on 30 June 2001 and flew to the Sun-Earth “L2 Lagrangian point”, arriving there on 1 October 2001. This lies at a ...
Improved stellar parameters of CoRoT-7
... models for this study. The atomic line data are extracted from VALD (Kupka et al. 1999), which is a collection from many different sources. The synthetic profiles are computed with synth (Valenti & Piskunov 1996). The VWA abundances are measured differentially with respect to a solar spectrum. We ha ...
... models for this study. The atomic line data are extracted from VALD (Kupka et al. 1999), which is a collection from many different sources. The synthetic profiles are computed with synth (Valenti & Piskunov 1996). The VWA abundances are measured differentially with respect to a solar spectrum. We ha ...
Chapter 15
... – Star formation begins at some random location in the galaxy creating a collection of stars – As these stars heat the gas around them and the larger ones explode, the disturbance sets off a star formation in an adjoining gas cloud – The process continues as long as there are enough large stars and ...
... – Star formation begins at some random location in the galaxy creating a collection of stars – As these stars heat the gas around them and the larger ones explode, the disturbance sets off a star formation in an adjoining gas cloud – The process continues as long as there are enough large stars and ...
Circum-stellar medium around rotating massive stars at solar
... identical to a spherical mesh with an equidistant angle discretisation and a logarithmic radial discretisation. With this mesh, the self-similar evolution phase of the bubble is well recovered, demonstrating the suitability of the chosen approach for the astrophysical problem under consideration (se ...
... identical to a spherical mesh with an equidistant angle discretisation and a logarithmic radial discretisation. With this mesh, the self-similar evolution phase of the bubble is well recovered, demonstrating the suitability of the chosen approach for the astrophysical problem under consideration (se ...