Quantifying the Relationship between Moreton–Ramsey Waves and “EIT Waves” Using Observations of Four Homologous Wave Events

Long, David M.; Jenkins, Jack; Valori, G.

doi:10.3847/1538-4357/ab338d

Cited by 18 publications

(31 citation statements)

References 66 publications

(62 reference statements)

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“…These values are consistent with observations of driven EUV waves relatively close to the source region, where the density increase resulting from the passage of a global EUV wave is much larger than the temperature increase (cf. Long et al 2019). They are also consistent with the interpretation of a global EUV wave as a large-amplitude, nonlinear wave or driven shock, as discussed by Long et al (2017b).…”

Section: Thermal Analysissupporting

confidence: 85%

“…The variation in density can then be estimated by assuming a line-of-sight length (estimated by Vanninathan et al 2015 to be ≈90 Mm). This length is consistent with the height calculated for global EUV waves including the 13 February 2009 event (Kienreich et al 2009;Patsourakos & Vourlidas 2009;Podladchikova et al 2019) and has been subsequently used by Long et al (2019). To enable a comparison here with Long et al (2019) and the simple tricolor method (Figure 11), we applied the DEM inversion method of Hannah & Kontar (2013) to the synthetic AIA data to two regions, one just outside the source region and one farther away, well within the quiet Sun along the wave path.…”

Section: Thermal Analysismentioning

confidence: 56%

“…The technique developed by Hannah & Kontar (2013) in particular has been used by multiple authors to examine the thermal evolution of global EUV waves and the response of the surrounding corona to the passage of a global EUV wave. Vanninathan et al (2015) found a temperature increase of ∼5%-6% and a density increase of ∼6%-9% for a global EUV wave observed by SDO/AIA on 15 February 2011 and identified the heating to take place at the frontal part of the wave, while Long et al (2019) found temperature (density) increases of 0.5%-1.1% (10%-26%) for four global EUV wave events occurring between 28-30 April 2014.…”

Section: Thermal Analysismentioning

confidence: 99%

“…The approach taken by both Vanninathan et al (2015) and Long et al (2019) is to calculate the DEM using an inversion code (in these case,s the technique developed by Hannah & Kontar 2013) and then integrate the DEM over all temperature bins to get an estimate of the change in temperature in a region of quiet Sun where the global EUV wave is shown to pass through. The variation in density can then be estimated by assuming a line-of-sight length (estimated by Vanninathan et al 2015 to be ≈90 Mm).…”

Section: Thermal Analysismentioning

confidence: 99%

“…In particular, interpretation of these features as MHD waves offers the opportunity to estimate the coronal magnetic field using coronal seismology techniques (see, e.g., Ballai 2007;West et al 2011;Kwon et al 2013;Long et al 2013, for previous work done on this topic). They are also closely associated with coronal mass ejections (CMEs) and can potentially provide insight into the direction and extent of the initial eruption (e.g., Temmer et al 2011;Möstl et al 2015;Long et al 2019). However, their derived properties, such as their kinematics, can be potentially biased by the techniques used to identify and track these features (cf., Byrne et al 2013), underlining the necessity for validation of these different techniques using a controlled data set with known properties.…”

Section: Introductionmentioning

confidence: 99%

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Validation of Global EUV Wave MHD Simulations and Observational Techniques

Downs

Warmuth

Long³

et al. 2021

ApJ

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Global EUV waves remain a controversial phenomenon more than 20 yr after their discovery by SOHO/EIT. Although consensus is growing in the community that they are most likely large-amplitude waves or shocks, the wide variety of observations and techniques used to identify and analyze them have led to disagreements regarding their physical properties and interpretation. Here, we use a 3D magnetohydrodynamic (MHD) model of the solar corona to simulate an EUV wave event on 2009 February 13 to enable a detailed validation of the various commonly used detection and analysis techniques of global EUV waves. The simulated event exhibits comparable behavior to that of a real EUV wave event, with similar kinematic behavior and plasma parameter evolution. The kinematics of the wave are estimated via visual identification and profile analysis, with both approaches providing comparable results. We find that projection effects can affect the derived kinematics of the wave, due to the variation in fast-mode wave speed with height in the corona. Coronal seismology techniques typically used for estimates of the coronal magnetic field are also tested and found to estimate fast-mode speeds comparable to those of the model. Plasma density and temperature variations of the wave front are also derived using a regularized inversion approach and found to be consistent with observed wave events. These results indicate that global waves are best interpreted as large-amplitude waves and that they can be used to probe the coronal medium using well-defined analysis techniques.

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Section: Thermal Analysissupporting

confidence: 85%

Section: Thermal Analysismentioning

confidence: 56%

Section: Thermal Analysismentioning

confidence: 99%

Section: Thermal Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Validation of Global EUV Wave MHD Simulations and Observational Techniques

Downs

Warmuth

Long³

et al. 2021

ApJ

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The formation of planetary systems with SPICA

Kamp

Honda

Nomura

et al. 2021

Publ. Astron. Soc. Aust.

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In this era of spatially resolved observations of planet-forming disks with Atacama Large Millimeter Array (ALMA) and large ground-based telescopes such as the Very Large Telescope (VLT), Keck, and Subaru, we still lack statistically relevant information on the quantity and composition of the material that is building the planets, such as the total disk gas mass, the ice content of dust, and the state of water in planetesimals. SPace Infrared telescope for Cosmology and Astrophysics (SPICA) is an infrared space mission concept developed jointly by Japan Aerospace Exploration Agency (JAXA) and European Space Agency (ESA) to address these questions. The key unique capabilities of SPICA that enable this research are (1) the wide spectral coverage $10{-}220\,\mu\mathrm{m}$ , (2) the high line detection sensitivity of $(1{-}2) \times 10^{-19}\,\mathrm{W\,m}^{-2}$ with $R \sim 2\,000{-}5\,000$ in the far-IR (SAFARI), and $10^{-20}\,\mathrm{W\,m}^{-2}$ with $R \sim 29\,000$ in the mid-IR (SPICA Mid-infrared Instrument (SMI), spectrally resolving line profiles), (3) the high far-IR continuum sensitivity of 0.45 mJy (SAFARI), and (4) the observing efficiency for point source surveys. This paper details how mid- to far-IR infrared spectra will be unique in measuring the gas masses and water/ice content of disks and how these quantities evolve during the planet-forming period. These observations will clarify the crucial transition when disks exhaust their primordial gas and further planet formation requires secondary gas produced from planetesimals. The high spectral resolution mid-IR is also unique for determining the location of the snowline dividing the rocky and icy mass reservoirs within the disk and how the divide evolves during the build-up of planetary systems. Infrared spectroscopy (mid- to far-IR) of key solid-state bands is crucial for assessing whether extensive radial mixing, which is part of our Solar System history, is a general process occurring in most planetary systems and whether extrasolar planetesimals are similar to our Solar System comets/asteroids. We demonstrate that the SPICA mission concept would allow us to achieve the above ambitious science goals through large surveys of several hundred disks within $\sim\!2.5$ months of observing time.

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Total reflection of a flare-driven quasi-periodic extreme ultraviolet wave train at a coronal hole boundary

Zhou

Shen

Tang

et al. 2022

A&A

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Context. A flare-driven quasi-periodic extreme ultraviolet wave train totally reflected at a coronal hole boundary was well imaged on both temporal and spatial scales by AIA/SDO. Aims. We aim to investigate the driving mechanisms of the quasi-periodic wave train and demonstrate the total reflection effect at the coronal hole boundary. Methods. The speeds of the incident and reflected wave trains are studied. The periodic correlation of the wave trains with the related flare is probed. We compare the measured incidence angle and the estimated critical angle. Results. We find that the periods of the incident and reflected wave trains are both about 100 s. The excitation of the quasi-periodic wave train was possibly due to the intermittent energy release in the associated flare since its period is similar to that of the quasi-periodic pulsations in the associated flare. Our observational results show that the reflection of the wave train at the boundary of the coronal hole was a total reflection because the measured incidence and critical angles satisfy the theory of total reflection: the incidence angle is smaller than the critical angle.

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Quantifying the Relationship between Moreton–Ramsey Waves and “EIT Waves” Using Observations of Four Homologous Wave Events

Cited by 18 publications

References 66 publications

Validation of Global EUV Wave MHD Simulations and Observational Techniques

Validation of Global EUV Wave MHD Simulations and Observational Techniques

The formation of planetary systems with SPICA

Total reflection of a flare-driven quasi-periodic extreme ultraviolet wave train at a coronal hole boundary

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