نتایج جستجو برای: corona wind
تعداد نتایج: 96504 فیلتر نتایج به سال:
Nonpulsed but variable X-ray emission has been detected from the binary system containing the radio pulsar PSR 1259–63 during two pointed ROSAT observations, taken five months apart. This 47.7 ms radio pulsar is in a highly eccentric (2 ∼ .85) binary system with the 10 to 15 M ̄ Be star SS2883. It is the first radio pulsar found to be in a binary system with a massive main sequence companion; it...
the amount of antibodies produced in colostrum following injection of the trivalent rota-corona virus and e. coli vaccine was evaluated to undrestand the priventive effects of vaccine against calf diarrhea. forthy six and 27 pregnant cows were selected from industrial dairy herds as a treatment and control groups, respectively in urmia iran. a 5 ml trivalent rota-corona virus and e .coli vaccin...
Understanding the physical processes responsible for accelerating the solar wind requires detailed measurements of the collisionless plasma in the extended solar corona. Some key clues about these processes have come from instruments that combine the power of an ultraviolet (UV) spectrometer with an occulted telescope. This combination enables measurements of ion emission lines far from the bri...
We present a series of models for the plasma properties along open magnetic flux tubes rooted in solar coronal holes, streamers, and active regions. These models represent the first self-consistent solutions that combine: (1) chromospheric heating driven by an empirically guided acoustic wave spectrum, (2) coronal heating from Alfvén waves that have been partially reflected, then damped by anis...
Ulysses plasma data at high heliographic latitudes were studied to develop constraints on the structure of the corona at the base of the high-speed solar wind. Salient features of the flow poleward of ±60◦ revealed: 1) low variances of all bulk flow parameters, 2) parameter values that agree with those measured during high-speed conditions in the ecliptic plane when all are scaled to 1AU, 3) th...
Fast streams of the solar wind with speeds of up to ≈ 800 km s−1 at a distance of 1 AU (astronomical unit) from the Sun are known to originate in solar coronal holes. With the Solar and Heliospheric Observatory (SOHO) detailed studies of the solar wind source regions have been made possible for the first time. We show images of solar polar coronal holes in the extreme ultraviolet (EUV), which w...
Context. To progress in the understanding of the solar wind and coronal dynamics, numerical modeling must include the transition region within the simulation domain, and not just as a bottom boundary. Published simulations including a transition region within the domain often do not take into account any modeling of the heat sources and sinks which generate the corona; in the rare self-consiste...
The solar corona expands non-uniformly into space as a supersonic plasma outflow known as the solar wind (Parker 1958). The solar wind carries signatures of coronal dynamics as well as locally generated turbulent phenomena, which span a broad range of scales. In situ spacecraft observations of fluctuations in solar wind parameters such as velocity and magnetic field (for example, Ruzmaikin et a...
The radiation spectra of many of the brightest ultraluminous X-ray sources (ULXs) are dominated by a hard power law component, likely powered by a hot, optically thin corona that Comptonizes soft seed photons emitted from a cool, optically thick black hole accretion disk. Before its dissipation and subsequent conversion into coronal photon power, the randomized gravitational binding energy resp...
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