PHYSICAL RESEARCH LABORATORY
... and 41Ca: Representative samples of first solar system solids? Astrophysical J. Letters 509, L137-140. 9. Sahijpal S., et al., (1998) A stellar origin for the short-lived nuclides in the early solar system. Nature 391, 559-561. 10. Goswami J.N., Sahijpal S., et al. (1998) In situ determination of io ...
... and 41Ca: Representative samples of first solar system solids? Astrophysical J. Letters 509, L137-140. 9. Sahijpal S., et al., (1998) A stellar origin for the short-lived nuclides in the early solar system. Nature 391, 559-561. 10. Goswami J.N., Sahijpal S., et al. (1998) In situ determination of io ...
2 Solar magnetic fields. - High Altitude Observatory
... Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots exist in spite of the fact that 100% of the solar luminosity is carried by turbulent convection that extends across the outer 30% of th ...
... Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots exist in spite of the fact that 100% of the solar luminosity is carried by turbulent convection that extends across the outer 30% of th ...
imaging_wkshp_all - Harvard-Smithsonian Center for Astrophysics
... acceleration of the plasma in the acceleration region of the solar wind. • Measured ion properties strongly suggest a specific type of (collisionless) waves in the Ion cyclotron resonance: corona to be damped: ion cyclotron waves with frequencies of 10 to 10,000 Hz. ...
... acceleration of the plasma in the acceleration region of the solar wind. • Measured ion properties strongly suggest a specific type of (collisionless) waves in the Ion cyclotron resonance: corona to be damped: ion cyclotron waves with frequencies of 10 to 10,000 Hz. ...
Efficiency improvement of crystalline silicon solar cells
... shape [15]. It has been reported in [16, 17] that the etching rate of <100> oriented crystal is higher than the <111> which leads to pyramid formation. In order to get uniform texturization, the surface preparation, process temperature, solution concentration, dosing rate and evaporation rate of IPA ...
... shape [15]. It has been reported in [16, 17] that the etching rate of <100> oriented crystal is higher than the <111> which leads to pyramid formation. In order to get uniform texturization, the surface preparation, process temperature, solution concentration, dosing rate and evaporation rate of IPA ...
Dating the Earliest Solids in our Solar System
... developed by Frank Shu (University of California, Berkeley), chondrules and CAIs formed near the Sun (at ~0.04-0.08 AU) by sunlight and radiation associated with solar flares and were transported later to the asteroid belt region by a bipolar outflow [see PSRD articles Relicts from the Birth of the ...
... developed by Frank Shu (University of California, Berkeley), chondrules and CAIs formed near the Sun (at ~0.04-0.08 AU) by sunlight and radiation associated with solar flares and were transported later to the asteroid belt region by a bipolar outflow [see PSRD articles Relicts from the Birth of the ...
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 ...
Grand Minima of Solar Activity and the Mean
... convection. Solar dynamo theory can explain at least the most basic features of the solar cycle. However, the temporal behavior of the large-scale solar magnetic field is more complex than just a regular cycle. From time to time in solar history cyclic solar activity became very weak or was even alm ...
... convection. Solar dynamo theory can explain at least the most basic features of the solar cycle. However, the temporal behavior of the large-scale solar magnetic field is more complex than just a regular cycle. From time to time in solar history cyclic solar activity became very weak or was even alm ...
1 LOCAL HELIOSEISMOLOGY OF NEAR
... indicates that the depth of detectable supergranular flows may be on the order of a few Mm. An analysis of near-surface flows over a solar rotation indicates that mature sunspots show supergranular sized outflows with peak velocities ∼300-500 m/s while almost all other types of magnetic regions show ...
... indicates that the depth of detectable supergranular flows may be on the order of a few Mm. An analysis of near-surface flows over a solar rotation indicates that mature sunspots show supergranular sized outflows with peak velocities ∼300-500 m/s while almost all other types of magnetic regions show ...
IRIS observations of the solar transition region
... Fully formed loops are seldom seen. Rather, loops appear to be lit up in segments, with each segment only being visible for roughly a minute. There is also a tendency for the UFS loops to appear to rise with time, as can be seen in ROI 2 (Fig. 1). We find that the UFS loops have a full length of 4 t ...
... Fully formed loops are seldom seen. Rather, loops appear to be lit up in segments, with each segment only being visible for roughly a minute. There is also a tendency for the UFS loops to appear to rise with time, as can be seen in ROI 2 (Fig. 1). We find that the UFS loops have a full length of 4 t ...
Written by G. Jeffrey Taylor
... with masses not too much different from the Sun reach this stage after using up all their hydrogen via nuclear fusion. Astrophysicists calculate that the nuclear environment in AGB stars would produce a 54Cr/52Cr ratio of about 1.1, substantially smaller than the 3.6 observed by Dauphas and coworker ...
... with masses not too much different from the Sun reach this stage after using up all their hydrogen via nuclear fusion. Astrophysicists calculate that the nuclear environment in AGB stars would produce a 54Cr/52Cr ratio of about 1.1, substantially smaller than the 3.6 observed by Dauphas and coworker ...
Summerschool Projects: Project 1: Sunspot data and solar cycle
... Task 4: Try to calibrate a monthly synoptic data set (dividing the images by the CLV, so that the contrast/brightness seems to be flat). Task 5: Derive the position of an active group (thresholding of the image). Follow the active group during one rotation and estimate the rotation periode of the Su ...
... Task 4: Try to calibrate a monthly synoptic data set (dividing the images by the CLV, so that the contrast/brightness seems to be flat). Task 5: Derive the position of an active group (thresholding of the image). Follow the active group during one rotation and estimate the rotation periode of the Su ...
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 ...
The Sun
... studied by monitoring waves caused by eathquakes Convection is source of waves in Sun On Sun’s surface, the waves appear as up and down oscillations of the gases, observed as Doppler shifts of ...
... studied by monitoring waves caused by eathquakes Convection is source of waves in Sun On Sun’s surface, the waves appear as up and down oscillations of the gases, observed as Doppler shifts of ...
Chapter 11 The Solar Wind
... Figure 11.1 shows the location on a Hertzsprung-Russell diagram of stars with high rates of mass loss. Hot, luminous stars with winds (including WolfRayet stars) are in the upper left; cool, luminous stars with winds are in the upper right. The approximate location of T Tauri stars on the H-R diagra ...
... Figure 11.1 shows the location on a Hertzsprung-Russell diagram of stars with high rates of mass loss. Hot, luminous stars with winds (including WolfRayet stars) are in the upper left; cool, luminous stars with winds are in the upper right. The approximate location of T Tauri stars on the H-R diagra ...
Observation of the Bastille day flare on 2000 July 14
... verify what theory I use, magnetic reconnection. ...
... verify what theory I use, magnetic reconnection. ...
Volume 11, Number 4 - RASC NB - Royal Astronomical Society of
... now, is of great interest to astronomers. They know there is a merger occurring, because the velocity of the hydrogen gas that envelopes the galaxies, is chaotic – as the galaxies merge, their gravities pull the gas in different directions. All this perturbation provides the fuel for bursts of star ...
... now, is of great interest to astronomers. They know there is a merger occurring, because the velocity of the hydrogen gas that envelopes the galaxies, is chaotic – as the galaxies merge, their gravities pull the gas in different directions. All this perturbation provides the fuel for bursts of star ...
Doubly Ionized Carbon Observed in the Plasma Tail of Comet Kudo
... with SOHO/Large Angle Spectroscopic Coronagraph (LASCO) light curves (10). In addition to the Ly ␣ and Ly  lines, we also observe emission from C III at 97.7 nm, the C II doublet at 103.6 and 103.7 nm, and three weak O I lines at 98.9, 99.0, and 102.7 nm (Fig. 2). (C III and C II are spectroscopic ...
... with SOHO/Large Angle Spectroscopic Coronagraph (LASCO) light curves (10). In addition to the Ly ␣ and Ly  lines, we also observe emission from C III at 97.7 nm, the C II doublet at 103.6 and 103.7 nm, and three weak O I lines at 98.9, 99.0, and 102.7 nm (Fig. 2). (C III and C II are spectroscopic ...
icso2000_picard
... before PDR ( launch in 2005-2007 window) Breadboard of active pointing carried in parallel The 2 EM of the Marconi/EEV CCD have been receipted and present excellent characteristics (dark current, flatness and ...
... before PDR ( launch in 2005-2007 window) Breadboard of active pointing carried in parallel The 2 EM of the Marconi/EEV CCD have been receipted and present excellent characteristics (dark current, flatness and ...
Here - HESPERIA
... University of Wuerzburg, D-97074 Wuerzburg, Germany The appearances of solar energetic particle events in interplanetary space around the Earth’s orbit, i.e., intensity-time profiles, anisotropies, energy spectra and elemental abundance ratios are determined by a combination of the underlying accele ...
... University of Wuerzburg, D-97074 Wuerzburg, Germany The appearances of solar energetic particle events in interplanetary space around the Earth’s orbit, i.e., intensity-time profiles, anisotropies, energy spectra and elemental abundance ratios are determined by a combination of the underlying accele ...
Stellar Spectroscopy during Exoplanet Transits
... * 3-D hydrodynamics studied in center-to-limb variations of line shapes, asymmetries and wavelength shifts * With sufficient S/N, also spectra of surface features such as starspots may become attainable ...
... * 3-D hydrodynamics studied in center-to-limb variations of line shapes, asymmetries and wavelength shifts * With sufficient S/N, also spectra of surface features such as starspots may become attainable ...
Fulltext PDF
... keep a close watch on the Sun and on its enigmatic faint outer atmosphere, the corona. Solar telescopes in space such as the Solar and Heliospheric Observatory (SOHO), the Transition Region and Coronal Explorer (TRACE) and Yohkoh satellite look at the Sun in x-ray, ultraviolet and other wavelengths ...
... keep a close watch on the Sun and on its enigmatic faint outer atmosphere, the corona. Solar telescopes in space such as the Solar and Heliospheric Observatory (SOHO), the Transition Region and Coronal Explorer (TRACE) and Yohkoh satellite look at the Sun in x-ray, ultraviolet and other wavelengths ...
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 ...
the amplitude of solar oscillations using stellar techniques
... not use the weights when calculating the HARPS power spectrum, since these were not available for BiSON and we wanted to make the window functions exactly the same. The amplitude of solar oscillations measured using the stellar technique is slightly lower than that measured by BiSON, by a factor of ...
... not use the weights when calculating the HARPS power spectrum, since these were not available for BiSON and we wanted to make the window functions exactly the same. The amplitude of solar oscillations measured using the stellar technique is slightly lower than that measured by BiSON, by a factor of ...
Solar observation
Solar observation is the scientific endeavor of studying the Sun and its behavior and relation to the Earth and the remainder of the Solar System. Deliberate solar observation began thousands of years ago. That initial era of direct observation gave way to telescopes in the 1600s followed by satellites in the twentieth century.