1,157 Photospheric PPTs View free & download

Understanding the Photospheric and Near-Photospheric Magnetic Field PowerPoint PPT Presentation

Understanding the Photospheric and Near-Photospheric Magnetic Field - So how does the convective dynamo model compare to observed X-ray fluxes in main-sequence stars? ... nests' to a magnetic picture of the large-scale dynamo ...

So how does the convective dynamo model compare to observed X-ray fluxes in main-sequence stars? ... nests' to a magnetic picture of the large-scale dynamo ...

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Photospheric flows around sunspots and pores PowerPoint PPT Presentation

Photospheric flows around sunspots and pores - Photospheric flows around sunspots and pores Michal Sobotka Astronomical Institute, Academy of Sciences of the Czech Republic, Ond ejov

Photospheric flows around sunspots and pores Michal Sobotka Astronomical Institute, Academy of Sciences of the Czech Republic, Ond ejov

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Photospheric MHD simulation of solar pores PowerPoint PPT Presentation

Photospheric MHD simulation of solar pores - Temperature at a fixed geometrical height (3 copies) Vertical Structure 2: ... log(Tau constant geometrical depth) Vertical magnetic field (Tau=1 surface) ...

Temperature at a fixed geometrical height (3 copies) Vertical Structure 2: ... log(Tau constant geometrical depth) Vertical magnetic field (Tau=1 surface) ...

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HMI, Photospheric Flows and ILCT PowerPoint PPT Presentation

HMI, Photospheric Flows and ILCT - Conformal deprojections, e.g., Mercator, locally preserve angles; scales are ... imposed differential rotation profile; red dots are raw velocities from Mercator ...

Conformal deprojections, e.g., Mercator, locally preserve angles; scales are ... imposed differential rotation profile; red dots are raw velocities from Mercator ...

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Finding Photospheric Flows with I LCT PowerPoint PPT Presentation

Finding Photospheric Flows with I LCT - Finding Photospheric Flows with I LCT. or,'Everything you always ... Space Sciences Lab, University of California. Outline. Context: ... by Stephane Regnier at ...

Finding Photospheric Flows with I LCT. or,'Everything you always ... Space Sciences Lab, University of California. Outline. Context: ... by Stephane Regnier at ...

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Magnetic Structure and Evolution of CMEs: From Their Photospheric Source Regions to the Heliosphere - Magnetic Structure and Evolution of CMEs: From Their Photospheric Source Regions to the Heliosphere

Magnetic Structure and Evolution of CMEs: From Their Photospheric Source Regions to the Heliosphere

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Photospheric Flows and Solar Flares PowerPoint PPT Presentation

Photospheric Flows and Solar Flares - Why investigate correlations between photospheric magnetic field & flares/CMEs? ... of average unsigned field |BR|, (mean, variance, skew, kurtosis), denoted M(|BR ...

Why investigate correlations between photospheric magnetic field & flares/CMEs? ... of average unsigned field |BR|, (mean, variance, skew, kurtosis), denoted M(|BR ...

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Diagnostics of flare activity level from turbulence parameters of photospheric plasma PowerPoint PPT Presentation

Diagnostics of flare activity level from turbulence parameters of photospheric plasma - Diagnostics of flare activity level from turbulence parameters of photospheric plasma ... non-linear dynamical system of magnetized plasma ...

Diagnostics of flare activity level from turbulence parameters of photospheric plasma ... non-linear dynamical system of magnetized plasma ...

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How are photospheric flows related to solar flares? PowerPoint PPT Presentation

How are photospheric flows related to solar flares? - uf is not equivalent to v; rather, uf vhor - (vn/Bn)Bhor ... Field and flow properties are ranked by distance from (0,0), the point of ...

uf is not equivalent to v; rather, uf vhor - (vn/Bn)Bhor ... Field and flow properties are ranked by distance from (0,0), the point of ...

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Connecting coronal structure to photospheric origins PowerPoint PPT Presentation

Connecting coronal structure to photospheric origins - vector field from a bipolar Active region (number 1731) on. February 21, 2002 ... This line profile is one of the first measurements of a 30G coronal magnetic field ...

vector field from a bipolar Active region (number 1731) on. February 21, 2002 ... This line profile is one of the first measurements of a 30G coronal magnetic field ...

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Diagnostics of the Interaction between Seismic Waves and Photospheric Magnetic Fields PowerPoint PPT Presentation

Diagnostics of the Interaction between Seismic Waves and Photospheric Magnetic Fields - Diagnostics of the Interaction between Seismic Waves and Photospheric ... Hannah Schunker. Ashley Crouch. Travel Time Signatures into Surface Magnetic Regions ...

Diagnostics of the Interaction between Seismic Waves and Photospheric ... Hannah Schunker. Ashley Crouch. Travel Time Signatures into Surface Magnetic Regions ...

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Using Simulations to Test Methods for Measuring Photospheric PowerPoint PPT Presentation

Using Simulations to Test Methods for Measuring Photospheric - Using Simulations to Test Methods for Measuring Photospheric. Velocity Fields ... et al. 2002 developed a method (dubbed MEF for 'Minimum Energy Fitting') whereby ...

Using Simulations to Test Methods for Measuring Photospheric. Velocity Fields ... et al. 2002 developed a method (dubbed MEF for 'Minimum Energy Fitting') whereby ...

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Signature of Avalanche in Solar Flares as Measured by Photospheric Magnetic Fields PowerPoint PPT Presentation

Signature of Avalanche in Solar Flares as Measured by Photospheric Magnetic Fields - Signature of Avalanche in Solar Flares as Measured by. Photospheric Magnetic Fields ... a solar flare, then certain signature of avalanche events might be seen ...

Signature of Avalanche in Solar Flares as Measured by. Photospheric Magnetic Fields ... a solar flare, then certain signature of avalanche events might be seen ...

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Using Photospheric Flows Estimated from Vector Magnetogram Sequences to Drive MHD Simulations PowerPoint PPT Presentation

Using Photospheric Flows Estimated from Vector Magnetogram Sequences to Drive MHD Simulations - ... determine Eh, and, via ideality, Ez. Equation (12) then determines ... Since and specify Eh, use ideality to specify Ez= - Eh Bh /Bz. Solve equation (12) for ...

... determine Eh, and, via ideality, Ez. Equation (12) then determines ... Since and specify Eh, use ideality to specify Ez= - Eh Bh /Bz. Solve equation (12) for ...

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AR8210: Using Data to Drive a Model Corona over Photospheric Timescales PowerPoint PPT Presentation

AR8210: Using Data to Drive a Model Corona over Photospheric Timescales - ... evolution of the vector magnetic field in the photosphere. ... Convective granulation pattern small compared to the size scale of AR at the photosphere ...

... evolution of the vector magnetic field in the photosphere. ... Convective granulation pattern small compared to the size scale of AR at the photosphere ...

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On the Origin of Strong Gradients in Photospheric Magnetic Fields PowerPoint PPT Presentation

On the Origin of Strong Gradients in Photospheric Magnetic Fields - Several studies correlated observations of impulsive solar activity flares and ... Each AR was tracked over 3 - 5 days, and cropped with a moving window. ...

Several studies correlated observations of impulsive solar activity flares and ... Each AR was tracked over 3 - 5 days, and cropped with a moving window. ...

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Flows and the Photospheric Magnetic Field Dynamics at Interior Corona Interface PowerPoint PPT Presentation

Flows and the Photospheric Magnetic Field Dynamics at Interior Corona Interface - HMI AIA, M1-H2: Mag. Activity. 2. The Store and Release Paradigm' (cf. ... (More on FLCT in M3: Mag. Data Products, Thurs. ... HMI AIA, M1-H2: Mag. Activity. 5 ...

HMI AIA, M1-H2: Mag. Activity. 2. The Store and Release Paradigm' (cf. ... (More on FLCT in M3: Mag. Data Products, Thurs. ... HMI AIA, M1-H2: Mag. Activity. 5 ...

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Photospheric emission models of GRBs and their detectability by GLAST PowerPoint PPT Presentation

Photospheric emission models of GRBs and their detectability by GLAST - this photosphere is expected to be blackbody. ... dissipative effects below the photosphere (magnetic reconnections or shocks) ...

this photosphere is expected to be blackbody. ... dissipative effects below the photosphere (magnetic reconnections or shocks) ...

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Solar-B X-ray Telescope (XRT) PowerPoint PPT Presentation

Solar-B X-ray Telescope (XRT) - Can a direct connection be established between coronal and photospheric events? Coronal Heating ... What are the relations to the photospheric magnetic fields? ...

Can a direct connection be established between coronal and photospheric events? Coronal Heating ... What are the relations to the photospheric magnetic fields? ...

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Observations and Modeling of Chromospheric Spicules PowerPoint PPT Presentation

Observations and Modeling of Chromospheric Spicules - Lockheed Martin Solar & Astrophysics Lab ... p-modes are evanescent... How do evanescent 5 min photospheric oscillations leak into the atmosphere? ...

Lockheed Martin Solar & Astrophysics Lab ... p-modes are evanescent... How do evanescent 5 min photospheric oscillations leak into the atmosphere? ...

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Energetic Particles in the Solar Atmosphere PowerPoint PPT Presentation

Energetic Particles in the Solar Atmosphere - Flares - relativistic electrons, ion beams, neutrons, pions ... respect to photospheric intersection of coronal magnetic separatrix surfaces (also, Demoulin, ...

Flares - relativistic electrons, ion beams, neutrons, pions ... respect to photospheric intersection of coronal magnetic separatrix surfaces (also, Demoulin, ...

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Solar Physics at Evergreen PowerPoint PPT Presentation

Solar Physics at Evergreen - How do magnetic waves carry energy from photospheric sound waves up into the chromosphere? ... Shorter-wavelength UV at higher altitudes, where chromosphere is hotter ...

How do magnetic waves carry energy from photospheric sound waves up into the chromosphere? ... Shorter-wavelength UV at higher altitudes, where chromosphere is hotter ...

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Distribution of the magnetic flux in elements of the magnetic field in an active region PowerPoint PPT Presentation

Distribution of the magnetic flux in elements of the magnetic field in an active region - ... in the photospheric plasma. Braiding and intertwining. of ... Modeling of interaction between turbulent plasma and the magnetic field below the photosphere: ...

... in the photospheric plasma. Braiding and intertwining. of ... Modeling of interaction between turbulent plasma and the magnetic field below the photosphere: ...

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Dopplergram from Filtergram FG Observation PowerPoint PPT Presentation

Dopplergram from Filtergram FG Observation - Narrowband Filter Imager (NFI) on SOT provides Dopplergrams (DGs) which are ... Observations with DGs are critically important in studies of photospheric ...

Narrowband Filter Imager (NFI) on SOT provides Dopplergrams (DGs) which are ... Observations with DGs are critically important in studies of photospheric ...

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Configuration of Magnetic Field in Solar Active Regions PowerPoint PPT Presentation

Configuration of Magnetic Field in Solar Active Regions - Helicity flows through the photosphere and the relationship with photospheric ... Development of magnetic shear and twist in AR10488 in the photosphere ...

Helicity flows through the photosphere and the relationship with photospheric ... Development of magnetic shear and twist in AR10488 in the photosphere ...

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V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode PowerPoint PPT Presentation

V.I. Abramenko, V.B. Yurchyshyn, H. Wang , T.R. Spirock, P.R. Goode - Photospheric plasma is in a state of highly developed turbulence, where ... Thus, we can apply methods of the theory of turbulence ...

Photospheric plasma is in a state of highly developed turbulence, where ... Thus, we can apply methods of the theory of turbulence ...

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NLTE Model Atmospheres for SuperSoft Xray Sources PowerPoint PPT Presentation

NLTE Model Atmospheres for SuperSoft Xray Sources - Spectral Energy Distributions for Hot Stars ... all stars with spectral type B or earlier. regarded as a domain of ... LS V 46 21. Photospheric abundances ...

Spectral Energy Distributions for Hot Stars ... all stars with spectral type B or earlier. regarded as a domain of ... LS V 46 21. Photospheric abundances ...

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Free Energies via Velocity Estimates PowerPoint PPT Presentation

Free Energies via Velocity Estimates - In ideal MHD, photospheric flows move mag-netic flux with a flux ... We used both LCT & ILCT to derive flows between pairs of boxcar- averaged m'grams. ...

In ideal MHD, photospheric flows move mag-netic flux with a flux ... We used both LCT & ILCT to derive flows between pairs of boxcar- averaged m'grams. ...

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Filament eruption related to largescale horizontal flows in the solar photosphere PowerPoint PPT Presentation

Filament eruption related to largescale horizontal flows in the solar photosphere - Filament eruption related to large-scale horizontal flows in the solar photosphere ... The influence of large-scale photospheric motions on the destabilization of an ...

Filament eruption related to large-scale horizontal flows in the solar photosphere ... The influence of large-scale photospheric motions on the destabilization of an ...

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Mapping Free Energy in the Solar Atmosphere PowerPoint PPT Presentation

Mapping Free Energy in the Solar Atmosphere - Depends on photospheric (Bx, By, Bz), (vx ,vy,vz), and (Bx(P), By(P) ... Longcope et al. (2005) quantified EUV loops' spatial and topological properties. ...

Depends on photospheric (Bx, By, Bz), (vx ,vy,vz), and (Bx(P), By(P) ... Longcope et al. (2005) quantified EUV loops' spatial and topological properties. ...

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Can magnetic waves in aurorae transform into acoustic waves Jada Maxwell PowerPoint PPT Presentation

Can magnetic waves in aurorae transform into acoustic waves Jada Maxwell - ... is crucial for transporting photospheric energy to the hot corona. ... Ofman, L. 'Alfv n waves in the solar corona, the solar wind, and the magnetosphere. ...

... is crucial for transporting photospheric energy to the hot corona. ... Ofman, L. 'Alfv n waves in the solar corona, the solar wind, and the magnetosphere. ...

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RosenbergColeman rule in ES data PowerPoint PPT Presentation

RosenbergColeman rule in ES data - ... of the photospheric field shows the 'butterfly' structure of the magnetic field ... Coronal field is too weak for the Zeeman effect. ...

... of the photospheric field shows the 'butterfly' structure of the magnetic field ... Coronal field is too weak for the Zeeman effect. ...

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Joint Discussion JD16 IHY Global Campaign Whole Heliosphere Interval PowerPoint PPT Presentation

Joint Discussion JD16 IHY Global Campaign Whole Heliosphere Interval - Relationships between the photospheric magnetic field, ... Babcock solar magnetograph using the Zeeman splitting of the 525.02 nm Fe I spectral line. ...

Relationships between the photospheric magnetic field, ... Babcock solar magnetograph using the Zeeman splitting of the 525.02 nm Fe I spectral line. ...

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Observations PowerPoint PPT Presentation

Observations - Coronagraph: 5 30 R_s FOV, Cadence ~ 1 hour. Thomson scattering of photospheric white light ... Very high cadence 1 m, and resolution ~ 700 km ...

Coronagraph: 5 30 R_s FOV, Cadence ~ 1 hour. Thomson scattering of photospheric white light ... Very high cadence 1 m, and resolution ~ 700 km ...

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SUBGROUP 1: Surface Solar Magnetic Fields PowerPoint PPT Presentation

SUBGROUP 1: Surface Solar Magnetic Fields - Can we infer the orientation of Bz of an ICME at 1 AU by focusing on the study ... A. Nindos: Examined chirality of source region using photospheric magnetograms ...

Can we infer the orientation of Bz of an ICME at 1 AU by focusing on the study ... A. Nindos: Examined chirality of source region using photospheric magnetograms ...

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- A means of specifying the photospheric boundary in a way consistent with the ... assume that ILCT or MEF flows permeate the entire layer, and implicitly solve ...

A means of specifying the photospheric boundary in a way consistent with the ... assume that ILCT or MEF flows permeate the entire layer, and implicitly solve ...

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COMPLEXITY IN SOLAR ACTIVE REGIONS PowerPoint PPT Presentation

COMPLEXITY IN SOLAR ACTIVE REGIONS - COMPLEXITY IN SOLAR ACTIVE REGIONS Loukas Vlahos Department of Physics University of Thessaloniki, Greece

COMPLEXITY IN SOLAR ACTIVE REGIONS Loukas Vlahos Department of Physics University of Thessaloniki, Greece

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Amir Levinson PowerPoint PPT Presentation

Amir Levinson - Title: No Slide Title Author: Amir Levinson Last modified by: Admin amir Created Date: 8/26/2002 1:03:38 PM Document presentation format: Pr sentation l' cran (4:3)

Title: No Slide Title Author: Amir Levinson Last modified by: Admin amir Created Date: 8/26/2002 1:03:38 PM Document presentation format: Pr sentation l' cran (4:3)

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Calculation of Intermittency in the Photosphere and Corona from Hinode Data PowerPoint PPT Presentation

Calculation of Intermittency in the Photosphere and Corona from Hinode Data - ... utilized 2D magnetic field images derived with Hinode SOT/FG ... Advantages: high resolution, high time cadence, uninterrupted measurements for several days ...

... utilized 2D magnetic field images derived with Hinode SOT/FG ... Advantages: high resolution, high time cadence, uninterrupted measurements for several days ...

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Prompt emission spectra from the photosphere of a GRB PowerPoint PPT Presentation

Prompt emission spectra from the photosphere of a GRB - ... spectra from the photosphere of a GRB. Dimitrios ... The equilibrium radius lies a factor of 10 below the photosphere ... The flow develops a hot photosphere ...

... spectra from the photosphere of a GRB. Dimitrios ... The equilibrium radius lies a factor of 10 below the photosphere ... The flow develops a hot photosphere ...

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Intermittency in the Photosphere and Corona as Derived from Hinode Data PowerPoint PPT Presentation

Intermittency in the Photosphere and Corona as Derived from Hinode Data - Title: Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions Last modified by: HSS Created Date: 5/10/2005 5:23:27 PM

Title: Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions Last modified by: HSS Created Date: 5/10/2005 5:23:27 PM

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Mapping Free Energy in the Solar Atmosphere - instability accord with this picture. (But cf. ... X-ray spectral radiance LX vs. total unsigned magnetic flux for solar and stellar objects. ...

instability accord with this picture. (But cf. ... X-ray spectral radiance LX vs. total unsigned magnetic flux for solar and stellar objects. ...

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B. T. Welsch (welsch@ssl.berkeley.edu) Space Sciences Lab, Univ. of California, Berkeley, CA 94720-7450 PowerPoint PPT Presentation

B. T. Welsch (welsch@ssl.berkeley.edu) Space Sciences Lab, Univ. of California, Berkeley, CA 94720-7450 - We used LCT to derive flows between pairs of boxcar-averaged magnetograms. ... Variance estimates were determined by shifting boxcar endpoints. ...

We used LCT to derive flows between pairs of boxcar-averaged magnetograms. ... Variance estimates were determined by shifting boxcar endpoints. ...

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The Effect of Sub-surface Fields on the Dynamic Evolution of a Model Corona PowerPoint PPT Presentation

The Effect of Sub-surface Fields on the Dynamic Evolution of a Model Corona - To model the evolution of the coronal magnetic field as eruptive events occur ... of the models by simulating known eruptive events and comparing model data with ...

To model the evolution of the coronal magnetic field as eruptive events occur ... of the models by simulating known eruptive events and comparing model data with ...

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A Data Driven Magnetohydrodynamic MHD Model of Active Region Evolution as a Tool for SDOHMI Data Ana PowerPoint PPT Presentation

A Data Driven Magnetohydrodynamic MHD Model of Active Region Evolution as a Tool for SDOHMI Data Ana - ... and density model to drive the model to obtain the following physical properties. ... This scheme achieves the second order accuracy both temporally and spatially. ...

... and density model to drive the model to obtain the following physical properties. ... This scheme achieves the second order accuracy both temporally and spatially. ...

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Statistical studies of the evolution of magnetic fields in the sun PowerPoint PPT Presentation

Statistical studies of the evolution of magnetic fields in the sun - Formation and evolution of active regions (photosphere) Coronal evolution of magnetic fields ... system (convection zone/photosphere/chromosphere/corona) is ...

Formation and evolution of active regions (photosphere) Coronal evolution of magnetic fields ... system (convection zone/photosphere/chromosphere/corona) is ...

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Sixth Solar-B Science Meeting PowerPoint PPT Presentation

Sixth Solar-B Science Meeting - Simulations taking on a new degree of realism. Beginnings of confrontation of ... Magneto-convection (both strong and weak field cases): detailed comparison of ...

Simulations taking on a new degree of realism. Beginnings of confrontation of ... Magneto-convection (both strong and weak field cases): detailed comparison of ...

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Observation of the Magnetic Field PowerPoint PPT Presentation

Observation of the Magnetic Field - Morphology and strength of B have been ... Emitted by magnetised photosphere, disk ... At the photosphere: Field topology may be more complicated than expected ...

Morphology and strength of B have been ... Emitted by magnetised photosphere, disk ... At the photosphere: Field topology may be more complicated than expected ...

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Incorporating%20Vector%20Magnetic%20Field%20Measurements%20into%20MHD%20models%20of%20the%20Solar%20Atmosphere PowerPoint PPT Presentation

Incorporating%20Vector%20Magnetic%20Field%20Measurements%20into%20MHD%20models%20of%20the%20Solar%20Atmosphere - Data-driven MHD models require an accurate time-series of vector ... Advantages of AR-8210 as a case study for numerical simulations: There exists quality vector data ...

Data-driven MHD models require an accurate time-series of vector ... Advantages of AR-8210 as a case study for numerical simulations: There exists quality vector data ...

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Solar Wind Structure in the Heliosphere: A Solar Perspective of Space Weather PowerPoint PPT Presentation

Solar Wind Structure in the Heliosphere: A Solar Perspective of Space Weather - flux expansion between photosphere and source surface (PFSS model) ... wind need to be traced back to the photosphere to determine the foot points. ...

flux expansion between photosphere and source surface (PFSS model) ... wind need to be traced back to the photosphere to determine the foot points. ...

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HMI - From 2D data arrays, f1(x1,x2) & f2(x1,x2), find vector flow v(x1,x2) consistent ... (2005, in prep): Use (i) 'minium structure' & (ii) 'coplanarity' assumptions, ...

From 2D data arrays, f1(x1,x2) & f2(x1,x2), find vector flow v(x1,x2) consistent ... (2005, in prep): Use (i) 'minium structure' & (ii) 'coplanarity' assumptions, ...

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Magnetic Flux Transport and the Hemispheric Pattern of Filaments PowerPoint PPT Presentation

Magnetic Flux Transport and the Hemispheric Pattern of Filaments - Magnetic Flux Transport and the Hemispheric Pattern of Filaments. Anthony Yeates1 ... a theory for the hemispheric pattern of filaments against observations. ...

Magnetic Flux Transport and the Hemispheric Pattern of Filaments. Anthony Yeates1 ... a theory for the hemispheric pattern of filaments against observations. ...

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X-ray Grating Spectroscopy PowerPoint PPT Presentation

X-ray Grating Spectroscopy - X-ray Photospheres Klaus Werner Institute for Astronomy and Astrophysics, University of T bingen, Germany

X-ray Photospheres Klaus Werner Institute for Astronomy and Astrophysics, University of T bingen, Germany

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CoronaPhotosphere Connection with Spectropolarimeter PowerPoint PPT Presentation

CoronaPhotosphere Connection with Spectropolarimeter - Corona B at photosphere. Global relation between AR corona and magnetic fields has been well studied. Magnetic Flux ... Non-uniformity in AR corona ...

Corona B at photosphere. Global relation between AR corona and magnetic fields has been well studied. Magnetic Flux ... Non-uniformity in AR corona ...

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Lecture 7 Element abundances PowerPoint PPT Presentation

Lecture 7 Element abundances - Then helium (He) was also formed in the Big Bang, when the Universe was 3 20 minutes old. The temperature was then just right ... Tolstoy's view in 1889 ' ...

Then helium (He) was also formed in the Big Bang, when the Universe was 3 20 minutes old. The temperature was then just right ... Tolstoy's view in 1889 ' ...

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The search for signatures of ion cyclotron resonance in the low corona PowerPoint PPT Presentation

The search for signatures of ion cyclotron resonance in the low corona - Photosphere. Spectroscopic observations. 2) origin of the dv2 -1/2 ... Photosphere. Resolution scale. LOS depth. 23. Are low q/m ions hotter than the others ? ...

Photosphere. Spectroscopic observations. 2) origin of the dv2 -1/2 ... Photosphere. Resolution scale. LOS depth. 23. Are low q/m ions hotter than the others ? ...

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Photospheric PowerPoint PPT Presentations