Alfvén Waves in the Solar Corona

By S. Tomczyk, S. McIntosh, S. Keil, P. Judge, T. Schad, D. Seeley, J. Edmondson. Science, 2007

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Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/efc4693b867448cf7e0e6e7680fa65859921f5ea

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Citations in the corpus

Decaying and decayless transverse oscillations of a coronal loop (2013, background): “…Nakariakov et al. 1999) or higher spatial harmonics (Verwichte et al. 2004; De Moortel & Brady 2007; Van Doorsselaere et al. 2007), but they have been observed as propagating waves in quiescent active regions (Tomczyk et al. 2007) and in supraarcades of flaring arcades (Verwichte et al. 2005).”
Alfvén Waves and Their Roles in the Dynamics of the Earth’s Magnetotail: A Review (2009, background): “…the magnetosphere of other planets (e.g., Acuna et al. 1981), and their role is being investigated to solve problems related to the solar wind (review by Tu and Marsch 1995), solar flares (e.g., Melrose 1992), the solar corona (e.g., Tomczyk et al. 2007), and the Earth’s core (Bloxham et al. 2002).”
Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, methodology): “…et al. 1999; Nakariakov et al. 1999), but it was not until several years later that reports were made of propagating kink waves in the corona by Tomczyk et al. (2007) using data from the Coronal Multi-Channel Polarimeter (CoMP).2 Typical periods are from several minutes to tens of minutes,…”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, background): “Alfvén waves which generate the ponderomotive force in the chromosphere have been much harder to detect (Van Doorsselaere et al., 2008), though see Erdélyi and Fedun (2007) and Tomczyk et al. (2007).”
Quasi-periodic Pulsations in Solar and Stellar Flares: An Overview of Recent Results (Invited Review) (2016, methodology): “rvations, we recommend a thorough reading of Nakariakov and Verwichte (2005) or De Moortel and Nakariakov (2012). More recently, it was found that kink waves are observed in nearly all coronal loops (Tomczyk et al., 2007; Van Doorsselaere, Nakariakov, and Verwichte, 2008; McIntosh et al., 2011; Nist”
Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology (2010, background): “…recently some studies reported the discovery of Alfvén waves, such as ubiquitous waves in the corona detected in the time series of Doppler images (Tomczyk et al. 2007; Tomczyk & McIntosh 2009), transverse waves in threadlike structure of solar prominences (Okamoto et al. 2007; Ning et al.…”
Detection of Waves in the Solar Corona: Kink or Alfvén? (2008, methodology): “[3] in Tomczyk et al. 2007) thus has to be multipliedFW with the filling factor as the observed waves cannot be planar.”
TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP (2009, methodology): “We concur with our earlier estimate (Tomczyk et al. 2007) that the energy carried in the resolved ubiquitous coronal waves is insufficient to heat the solar corona by at least three to four orders of magnitude.”
PROPAGATING WAVES ALONG SPICULES (2011, methodology): “…transverse waves propagating in the corona have been reported using line-of-sight Dopplergrams from ground-based coronagraphs (Sakurai et al. 2002; Tomczyk et al. 2007; Tomczyk & McIntosh 2009) and spectrometers in orbit (Banerjee et al. 2010; McIntosh et al. 2011, and references therein).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “Alfvén waves have indeed been observed both in the chromosphere (De Pontieu et al. 2007b) and in the corona (e.g., Tomczyk et al. 2007).”
Alfvén Waves in the Solar Atmosphere (2012, methodology): “Tomczyk et al. (2007) suggested that these oscillations are the signatures of Alfvén waves in the corona for the following reasons: (a) The waves have phase speeds of about 2000 km s−1, which is considerably higher than the coronal sound speed, (b) The waves propagate along density structures that…”
CORONAL LOOP OSCILLATIONS OBSERVED WITH ATMOSPHERIC IMAGING ASSEMBLY—KINK MODE WITH CROSS-SECTIONAL AND DENSITY OSCILLATIONS (2011, background): “…(Ofman et al. 1997) and Hinode (Erdelyi & Taroyan 2008), EIT/SOHO (DeForest & Gurman 1998), and TRACE (De Moortel et al. 2002a, 2002b), fast Alfvénic waves with SECIS (Williams et al. 2001; Katsiyannis et al. 2003), or fast kink waves with TRACE (Verwichte et al. 2004; Tomczyk et al. 2007).”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, background): “For example, convective photospheric motions inevitably launch low-frequency Alfvén waves into the corona by perturbing the footpoints of open magnetic field lines, and low-frequency Alfvén waves are observed in the corona (Tomczyk et al. 2007) and atr > 0.3 AU (Belcher and Davis 1971).”