TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP

By S. Tomczyk, S. McIntosh. 2009

224 citations recorded by the source corpus.

We employ a sequence of Doppler images obtained with the Coronal Multi-channel Polarimeter (CoMP) instrument to perform time–distance seismology of the solar corona. We construct the first k–ω diagrams of the region. These allow us to separate outward and inward propagating waves and estimate the spatial variation of the plane-of-sky-projected phase speed, and the relative amount of outward and inward directed wave power. The disparity between outward and inward wave power and the slope of the observed power-law spectrum indicate that low-frequency Alfvénic motions suffer significant attenuation as they propagate, consistent with isotropic MHD turbulence.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4d6411d16b12e54c268b2a3e02a757ed10b27d72

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In Astronomy and Astrophysics

Citations in the corpus

Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology (2010, background): “…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. 2009), and the transverse…”
The Interface Region Imaging Spectrograph (IRIS) (2012, background): “…transverse and torsional (Alfvénic) motions have now been measured in the chromosphere and corona (Tomczyk et al., 2007; De Pontieu et al., 2007a; Tomczyk and McIntosh, 2009; McIntosh et al., 2011; Liu et al., 2011; De Pontieu et al., 2012; Wedemeyer-Böhm et al., 2012; Su et al., 2013;…”
Geoeffective Properties of Solar Transients and Stream Interaction Regions (2017, background): “This is attributed to Alfvénic fluctuations in the following HSSs (e.g., Tsurutani and Gonzalez 1987; Balogh et al. 1995; Tsurutani et al. 1995; Lucek and Balogh 1998) that ultimately originate from the Sun and propagate along open field lines into the heliosphere (e.g., Tomczyk and McIntosh 2009).”
Alfvén Waves in the Solar Atmosphere (2012, background): “In a follow up investigation, Tomczyk & McIntosh (2009) performed time-distance seismology of the solar corona, and constructed a k–ω diagram of the region.”
Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, methodology): “In that sense, the larger field of view of CoMP had the advantage of determining whether the kink waves are propagating or not, but certainly the presence of non-flare and non-CME generated low amplitude kink waves was confirmed independently by both instruments.”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “The authors compared the velocity power spectrum measured from Coronal Multi-channel Polarimeter (CoMP; Tomczyk et al. 2008) observations of quiescent coronal loops (Tomczyk and McIntosh 2009) to the chromospheric velocity power spectrum of fibrils.”
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).”
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “Fourier analysis of wave power and dispersion relation with k–ω diagrams is a common technique in helioseismology, but was previously underused in coronal seismology mainly because of the scarcity of high-cadence data (DeForest, 2004; Tomczyk and McIntosh, 2009).”