نتایج جستجو برای: chromosphere

تعداد نتایج: 926  

Journal: :The Astronomical Journal 1955

Journal: :Symposium - International Astronomical Union 1998

Journal: :Monthly Notices of the Royal Astronomical Society 1933

Journal: :Science 2007
Kazunari Shibata Tahei Nakamura Takuma Matsumoto Kenichi Otsuji Takenori J Okamoto Naoto Nishizuka Tomoko Kawate Hiroko Watanabe Shin'ichi Nagata Satoru Ueno Reizaburo Kitai Satoshi Nozawa Saku Tsuneta Yoshinori Suematsu Kiyoshi Ichimoto Toshifumi Shimizu Yukio Katsukawa Theodore D Tarbell Thomas E Berger Bruce W Lites Richard A Shine Alan M Title

The heating of the solar chromosphere and corona is a long-standing puzzle in solar physics. Hinode observations show the ubiquitous presence of chromospheric anemone jets outside sunspots in active regions. They are typically 3 to 7 arc seconds = 2000 to 5000 kilometers long and 0.2 to 0.4 arc second = 150 to 300 kilometers wide, and their velocity is 10 to 20 kilometers per second. These smal...

2008
Hugh S. Hudson

In this topical review I revisit the “chromospheric flare”. This should currently be an outdated concept, because modern data seem to rule out the possiblity of a major flare happening independently in the chromosphere alone, but the chromosphere still plays a major observational role in many ways. It is the source of the bulk of a flare’s radiant energy – in particular the visible/UV continuum...

2014
M. SOBOTKA M. ŠVANDA J. JURČÁK P. HEINZEL D. DEL MORO F. BERRILLI

Several mechanisms may heat the solar chromosphere: acoustic waves, magnetoacoustic waves (slow, fast, and Alfvén waves), and small-scale magnetic reconnections. Based on observations in the Ca II 854.2 nm line, the contribution of acoustic waves to the heating of quiet and plage regions in the chromosphere is discussed. The energy released by radiative losses is compared with the energy deposi...

Journal: :Monthly Notices of the Royal Astronomical Society 1929

Journal: :The Astronomical Journal 1957

2002
Mats Carlsson

We investigate the ionization of hydrogen in a dynamic Solar atmosphere. The simulations include a detailed non-LTE treatment of hydrogen, calcium and helium but lack other important elements. Furthermore, the omission of magnetic fields and the one-dimensional approach make the modeling unrealistic in the upper chromosphere and higher. We discuss these limitations and show that the main result...

2009
J. Martin Laming

We revisit in more detail a model for element abundance fractionation in the solar chromosphere, that gives rise to the “FIP Effect” in the solar corona and wind. Elements with first ionization potential below about 10 eV, i.e. those that are predominantly ionized in the chromosphere, are enriched in the corona by a factor 3-4. We model the propagation of Alfvén waves through the chromosphere u...

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