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YbV 3 Sb 4 and EuV 3 Sb 4 vanadium-based kagome metals with Yb 2+ and Eu 2+ zigzag chains
Here, in this work, we present YbV 3 Sb 4 and EuV 3 Sb 4 , two compounds exhibiting slightly distorted vanadium-based kagome nets interleaved with zigzag chains of divalent Yb 2+ and Eu 2+ ions. Single crystal growth methods are reported alongside magnetic, electronic, and heat capacity measurements. YbV 3 Sb 4 is a nonmagnetic metal with no collective phase transitions observed between 60 mK and 300 K. Conversely, EuV 3 Sb 4 is a magnetic kagome metal exhibiting easy-plane ferromagneticlike order below T C =32 K with hints of modulated spin texture under low field. With YbV 3 Sb 4 and EuV 3 Sb 4 we demonstrate another direction for the discovery and development of vanadium-based kagome metals while incorporating the chemical and magnetic degrees of freedom offered by a rare-earth sublattice.
Three-dimensional modeling of EUV photoresist using the multivariate Poisson propagation model
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Inspection of next generation EUV resists with nano-projectile SIMS
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EUV and Plasma Sources using High Energy Solid State ¿ = 2¿m laser drivers
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EUV and Plasma Sources using High Energy Solid State lambda = 2(mu)m laser drivers
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High Energy Solid-State 2um Laser Drivers for Efficient EUV and Plasma Sources
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Inference of magnetic field in the coronal streamer invoking kink wave motions generated by multiple EUV waves
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On the determination of solar EUV emission altitudes using the earth as an occulting disk
Determination of solar extreme ultraviolet emission altitudes by using earth as occulting disk
Earth as an occulting disk for study of solar EUV emission heights.
Source distributions of UV and X-ray emission in corona and chromosphere determined from flight of spacecraft-borne instruments into Earth shadow
The response of the upper atmospheric temperature to changes in solar EUV RADIATION and geomagnetic activity
Upper atmospheric temperature response to changes in solar extreme ultraviolet radiation and geomagnetic activity
The response of the upper atmospheric temperature to changes in solar EUV radiation and geomagnetic activity
Solar radiation and magnetic effects on upper atmospheric neutral temperatures derived from satellite drag
The response of the upper atmospheric temperature to changes in solar EUV radiation and geomagnetic activity.
Upper atmosphere temperature variations analysis from satellite drag observations, discussing solar far UV and geomagnetic activity roles
Calibration changes in EUV solar satellite instruments
Absolute photometric calibration of solar satellite instruments in extreme ultraviolet region
EUV observations of the chromospheric network.
Extreme ultraviolet observations of a quiet region of the sun on Aug. 18, 1969, with the Harvard spectroheliometer on OSO 6 indicate that the chromospheric network can be observed in lines of the chromosphere and transition region (T = 840,000 K) with almost identical structure. At coronal heights, the network changes but some residual structure can still be discerned in Mg X and perhaps Si XII, although there is little or no evidence remaining in Fe XVI.
Broad band solar EUV absorption in the earth's upper atmosphere.
Observation data on solar radiation intensity, based on measurements performed as a function of time for three broad wavelength bands between 280 and 1030 A by a wheel spectrometer on Oso 5 during sunrise and sunset, are compared with predicted intensity variations based on Cira models. The differences between sunrise and sunset data, as well as those between observed and predicted data are discussed.
High resolution rocket EUV solar spectrograph.
The design and performance of an Aerobee 150 rocket-borne solar spectrograph covering a wavelength range of 10 to 385 A are discussed. The spectrograph uses a gold-coated replica concave grating of 3-m radius with 1200 grooves/mm at an angle of incidence of 88 deg. The spectra are recorded on glass photographic plates making possible wavelength determination to 0.003 A if known standard wavelengths occur frequently enough. Special attention to scattered light made possible the photographing of the solar spectrum from 60 to 385 A without using filters to absorb the strong visible and UV sunlight, although the solar spectrum was also recorded through metal foil filters. In the laboratory the spectrograph has been used to record spectra of highly ionized metals with a resolution of 0.03 A or better.
An investigation of the structure and composition of the solar atmosphere using X-ray and EUV spectra obtained with the OV1-17 and OSO-4 and OSO-5 satellites
Studies of the structure and composition of the solar corona were undertaken, using a number of satellite observations of the coronal X-ray spectrum. A systematic technique was developed to carry out the required analysis, and the analytical techniques available to calculate the coronal spectrum have been developed and improved. A review of other analyses of solar coronal structure is also included.