Thompson B. Role of plasmoid ejections in solar flare energy release. Tokyo Studies of transient brightenings microflares discovered in solar active regions. Bookbinder and E. Coronal structure and temperature. StCyr, J. Burkepile, O. White, T. Kucera, N. Nitta, Y. Hanaoka, P.
Mein, J. IAU Coll. Uchida, T. Kosugi, and H. Hudson , p. Pallavicini and A. Winterhalter, J. Gosling, S. Habbal, W. Kurth, and M. Yohkoh Conference, held in Bath, England, March , eds. Bentley and J. Taylor and J.
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Conference, held in Greenbelt, Maryland, Aug , eds. Ramaty, N.
Mandzhavidze, and X. Yamashita and T. Watanabe , Universal Academy Press, Tokyo, p. Stationary post-flare giant arches. Mariska , ASP, San Francisco, California, Properties of thermal flares MK derived from observations: does a reconnection mechanism have a role in the flare process. Tokyo Structures and heating mechanisms of the solar corona. Mariska , ASP, San Francisco, California, A coronal velocity field around a long-duration event: search for reconnection inflow. L, Hoeksema,J. Workshop held in Santa Fe, New Mecico, , eds.
Hansen and R. Gamma-ray observations with the Yohkoh satellite. Workshop, ed. Makino , Universal Academy Press, Tokyo, The dynamic solar corona in X-ray with Yohkoh. Mariska , ASP, San Francisco, California, Yohkoh evidence against the reclosing opened-up arcade model for arcade flares and arcade formations.
Dynamics and heterogeneities in post-flare loops. Kuhn and M. Penn , World Scientific, Singapore, 45 Association of solar coronal temperature and structure from ground-based emission-line data with global magnetic field models and Yohkoh SXT data. Colorado, Boulder, Colorado A multispectral study of the flare of July 16, using data from the Owens Valley Solar Array and instruments from the Yohkoh spacecraft.
Siegmund and J. Workshop, Workshop, Dunhuang, China, Sept , eds.
Solar Neutrons and Related Phenomena | Lev Dorman | Springer
Academic Publishers, Bejing, 27 Soft and hard X-ray observations of flares from Yohkoh: magnetic structure and energy release. Academic Publishers, Bejing, Temperature structures of the active-region corona revealed with Norikura coronagraph and Yohkoh soft X-ray telescope. Also Lecture Notes in Physics, volume , Characteristics of two simple microwave bursts.
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Spectral signatures of electron-beam-heated atmospheres. Academic Publishers, Bejing, Loop-top hard X-ray source as evidence for reconnection above a soft X-ray loop in solar flares.
Watanabe Ta. Academic Publishers, Bejing, Microflares: Detailed comparisons between soft X-ray images and high resolution magnetograms. The isothermal approximation: application of various atomic data. Academic Publishers, Bejing, Structure and dynamics of magnetic reconnection in the solar corona.
Oya , Coronal activity observed by Yohkoh Invited Review. Hiei and J. Culhane , Elsevier Science, Magnetodynamic phenomena in the corona as revealed by Yohkoh. Kofu Symposium, held in Kofu, Sept , eds. Enome and T. Yohkoh soft X-ray observations of the June flare. Sakurai, T. Hirayama, and G. S, Nitta,N. Ryan and W. Tokyo A systematic study of temporal and spectral variations of solar flare hard X-ray morphology.
Yohkoh observations relevant to mass ejection. Metric type III bursts from flaring X-ray bright points.
CA United States Wave heating of the solar corona. Be the first to write a review. Add to Wishlist.
Ships in 15 business days. Link Either by signing into your account or linking your membership details before your order is placed. Description Table of Contents Product Details Click on the cover image above to read some pages of this book!
Lev I Dorman
Industry Reviews From the reviews: "This book represents an exhausting monograph on solar neutrons written by an expert who worked about these particles from the Sun since The table of contents is a very detailed one, it covers 24 printed pages. Many observations are given in tables and figures, the corresponding theoretical developments are given in many formulas, and subject index and reference list are carefully developed. The Solar Neutron Decay Phenomenon.
More Books in Astrophysics See All. Apollo 11 : The Inside Story. In Stock. This appears to hold almost universally over a broad range of physical conditions Kroupa, This is itself very different from the case of Pop III, where even small changes to the properties of host halos result in stellar masses that can vary by up to two orders of magnitude Hirano et al.
How and when did this transition in star formation take place? In their supernova explosions, Pop III stars introduced the first heavy elements metals to the universe. The addition of metals to a gas adds to the number of atomic and molecular transitions, increasing its ability to cool. Recalling that, to first order, Pop III stars are massive because metal-free gas clouds cease to cool and, thus, fragment as they collapse, one can then calculate the additional metals required for cooling and fragmentation to continue.
Numerous studies using three-dimensional simulations of homogeneously enriched gas clouds have shown that fragmentation does occur at these critical metallicities Bromm et al. For example, Figure 3 shows density projections from Enzo simulations of gas clouds at different metallicities from Smith et al. Additionally, Smith et al.
However, other simulations claimed that the ability of gas to fragment was extremely dependent on the initial setup of the simulation Jappsen et al. For example, simulations without rotation or turbulence in the cloud show no fragmentation at any metallicity.
The only way to resolve this is to understand the true initial conditions of the first low mass stars. Figure 3. Density projections of the central 0.