The Ozone Monitoring Instrument (OMI) onboard the NASA EOS Aura spacecraft is a nadir viewing spectrometer that measures solar reflected and backscattered light in a selected range of the ultraviolet and visible spectrum. The instrument has a 2600 km wide viewing swath and it is capable of daily, global contiguous mapping. We have developed and implemented a surface ultraviolet irradiance algor...

Carbon nanotube-In2O3 nanocomposites were synthesized by sol-gel method with the help of ultrasonic radiation. The samples were characterized by X-ray diffractometer, transmission electron microscopy and energy dispersive spectrometer. The UV absorbing properties were detected by the UV spectrophotometer. Photo degradation of methylene blue in aqueous solution was investigated by using CNT/In2O...

Many workers perform their daily activities outdoors undertaking different postures and many anatomical body sites are UVR exposed. This paper aims to compare the anatomical distribution of the solar erythemal UVR to the higher half of the body for farm workers during their usual working activity in agriculture. This research was carried out in the experimental farm“Azienda Agraria Didattico-Sp...

The present spectroscopic study of the ultraviolet coronal emission in a polar hole, detected on April 6–9, 1996 with the Ultraviolet Coronagraph Spectrometer aboard the SOHO spacecraft, identifies the inter–plume lanes and background coronal hole regions as the channels where the fast solar wind is preferentially accelerated. In inter–plume lanes, at heliocentric distance 1.7 R ⊙ , the corona ...

Carbon monoxide (CO) is a sensitive tracer of the thermal profile and winds in Mars' middle atmosphere chemistry that balances CO2 whole Mars. The Emirates Ultraviolet Spectrometer (EMUS) onboard Mars Mission Hope probe images at ultraviolet wavelengths from approximately 100 to 170 nm. ?CO/CO2, column density ratio CO carbon dioxide, provides measure relative variability within Martian thermos...

We present in this Letter the first coordinated radio occultation measurements and ultraviolet observations of the inner corona below 5.5 Rs, obtained during the Galileo solar conjunction in January 1997, to establish the origin of the slow solar wind. Limits on the flow speed are derived from the Doppler dimming of the resonantly scattered component of the oxygen 1032 Å and 1037 Å lines as mea...

The widths of spectral lines in the ultraviolet (UV) and extreme ultraviolet (EUV) spectral regions that are formed in the solar transition region and corona are usually greater than the optically thin widths due to thermal Doppler broadening calculated under the assumption of ionization equilibrium. Although opacity can explain the widths of some lines, there are a host of optically thin lines...

20375 Received ; accepted – 2 – ABSTRACT We present in this Letter the first coordinated radio occultation measurements and ultraviolet observations of the inner corona below 5.5 R s , obtained during the Galileo solar conjunction in January 1997, to establish the origin of the slow solar wind. Limits on the flow speed are derived from the Doppler dimming of the resonantly scattered component o...