@Article{RemyaTsReLaFaEcGl:2014:LoPlBe,
               author = "Remya, B. and Tsurutani, B. T. and Reddy, R. V. and Lakhina, G. S. 
                         and Falkowski, B. J. and Echer, Ezequiel and Glassmeier, K. -H.",
          affiliation = "Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India. and 
                         CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. and Indian Inst 
                         Geomagnetism, Navi Mumbai, Maharashtra, India. and Indian Inst 
                         Geomagnetism, Navi Mumbai, Maharashtra, India. and CALTECH, Jet 
                         Prop Lab, Pasadena, CA 91109 USA. and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and IGEP, D-38106 Braunschweig, 
                         Germany.",
                title = "Large-amplitude, circularly polarized, compressive, obliquely 
                         propagating electromagnetic proton cyclotron waves throughout the 
                         earth's magnetosheath: low plasma beta conditions",
              journal = "Astrophysical Journal",
                 year = "2014",
               volume = "793",
               number = "1",
                month = "Sep.",
             keywords = "instabilities, methods: data analysis, planets and satellites: 
                         individual (Earth, Cassini, WIND), planets and satellites: 
                         magnetic fields, polarization.",
             abstract = "During 1999 August 18, both Cassini and WIND were in the Earth's 
                         magnetosheath and detected transverse electromagnetic waves 
                         instead of the more typical mirror-mode emissions. The Cassini 
                         wave amplitudes were as large as similar to 14 nT (peak to peak) 
                         in a similar to 55 nT ambient magnetic field B-0. A new method of 
                         analysis is applied to study these waves. The general wave 
                         characteristics found were as follows. They were left-hand 
                         polarized and had frequencies in the spacecraft frame (f(scf)) 
                         below the proton cyclotron frequency (f(p)). Waves that were 
                         either right-hand polarized or had f(scf) > f(p) are shown to be 
                         consistent with Doppler-shifted left-hand waves with frequencies 
                         in the plasma frame f(pf) < f(p). Thus, almost all waves studied 
                         are consistent with their being electromagnetic proton cyclotron 
                         waves. Most of the waves (similar to 55\%) were found to be 
                         propagating along B0 (theta(kB0) < 30 degrees), as expected from 
                         theory. However, a significant fraction of the waves were found to 
                         be propagating oblique to B0. These waves were also circularly 
                         polarized. This feature and the compressive ([B-max - 
                         B-min]/B-max, where B-max and B-min are the maximum and minimum 
                         field magnitudes) nature (ranging from 0.27 to 1.0) of the waves 
                         are noted but not well understood at this time. The proton 
                         cyclotron waves were shown to be quasi-coherent, theoretically 
                         allowing for rapid pitch-angle transport of resonant protons. 
                         Because Cassini traversed the entire subsolar magnetosheath and 
                         WIND was in the dusk-side flank of the magnetosheath, it is 
                         surmised that the entire region was filled with these waves. In 
                         agreement with past theory, it was the exceptionally low plasma 
                         beta (0.35) that led to the dominance of the proton cyclotron wave 
                         generation during this interval. A high-speed solar wind stream (< 
                         V-sw > = 598 km s(-1)) was the source of this low-beta plasma.",
                  doi = "10.1088/0004-637X/793/1/6",
                  url = "http://dx.doi.org/10.1088/0004-637X/793/1/6",
                 issn = "0004-637X and 1538-4357",
                label = "isi 2014-11 RemyaTsReLaFaEcGl:2014:LOPLBe",
             language = "en",
           targetfile = "0004-637X_793_1_6remya.pdf",
        urlaccessdate = "27 abr. 2024"
}