Relative Abundance Measurements in Plumes and Interplumes

Guennou, C.; Hahn, Michael; Savin, D. W.

doi:10.1088/0004-637x/807/2/145

Cited by 10 publications

(15 citation statements)

References 51 publications

(77 reference statements)

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“…That the FIP effect may depend on the time elements have been confined within a structure has been suggested by, e.g., Feldman and Widing (2003): this might possibly account for the different values obtained by different authors. A recent paper, Guennou et al (2015), further supports this hypothesis. These authors give values of relative element abundances in plumes and interplume regions, inferred from HINODE/EIS off-limb observations acquired in March 2007.…”

Section: Fip Effect In Plumes?mentioning

confidence: 65%

“…Unfortunately, the data do not include lines from high-FIP elements and the FIP bias has been evaluated from the ratio of Fe and Si to S abundance, S being a moderate-FIP element (the sulphur FIP being ≈ 10.36 eV). Over 24-hour observations, one of the plume analyzed by Guennou et al (2015) revealed a decrease of the FIP bias, while other plumes (and interplume regions) have values independent of time. Guennou et al (2015) suggest this effect is related to the phase of the BP lifetime when plumes form above the associated BP, possibly plumes being representative of the abundances of the bright point.…”

Section: Fip Effect In Plumes?mentioning

confidence: 96%

“…Over 24-hour observations, one of the plume analyzed by Guennou et al (2015) revealed a decrease of the FIP bias, while other plumes (and interplume regions) have values independent of time. Guennou et al (2015) suggest this effect is related to the phase of the BP lifetime when plumes form above the associated BP, possibly plumes being representative of the abundances of the bright point. The topic is still open to discussion and can be the subject of future research.…”

Section: Fip Effect In Plumes?mentioning

confidence: 96%

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Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL) images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV) and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: Fip Effect In Plumes?mentioning

confidence: 65%

Section: Fip Effect In Plumes?mentioning

confidence: 96%

Section: Fip Effect In Plumes?mentioning

confidence: 96%

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Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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“…Notes: (1) name given by NED (LCDCS clusters come from Gonzalez et al 2001), (2) right ascension in degrees (J2000.0), (3) declination in degrees (J2000.0), (4) redshift, (5) number of galaxies with redshifts in the cluster range, (6) useful XMM-Newton exposure time (in seconds), (7) temperature of the X-ray gas, (8) X-ray luminosity in the [0.5,8.0] keV band, (9) X-ray gas mass in the r 500 radius, (10) total mass in the r 500 radius, (11) subtructure inside the cluster (1 means yes, -1 means no, 0 means not detectable with data in hand). ** The position given for LCDCS 504 comes from Guennou et al (2013) where we determined the centre as the position of the cD, whereas the position given in parentheses was obtained from NED. *** The cluster MACS J1423.8+2404 did not have any XMM-Newton public data, but we collected Chandra data with enough depth to be able to subtract a β−model and search for substructures.…”

Section: Basic Parametersmentioning

confidence: 99%

“…Gemini/GMOS spectroscopy has a resolution of 7 Å/px (see Guennou et al 2013 for details). The targeted objects were brighter than I AB ∼ 24, and the reduction was made with the IRAF package and the Gemini/Gmos environment.…”

Section: Optical Data and Serna And Gerbal Analysismentioning

confidence: 99%

Structure and substructure analysis of DAFT/FADA galaxy clusters in the [0.4–0.9] redshift range

Guennou

Adami

Durret

et al. 2014

A&A

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Context. The DAFT/FADA survey is based on the study of ∼90 rich (masses found in the literature >2 × 10 14 M ) and moderately distant clusters (redshifts 0.4 < z < 0.9), all with HST imaging data available. This survey has two main objectives: to constrain dark energy (DE) using weak lensing tomography on galaxy clusters and to build a database (deep multi-band imaging allowing photometric redshift estimates, spectroscopic data, X-ray data) of rich distant clusters to study their properties. Aims. We analyse the structures of all the clusters in the DAFT/FADA survey for which XMM-Newton and/or a sufficient number of galaxy redshifts in the cluster range are available, with the aim of detecting substructures and evidence for merging events. These properties are discussed in the framework of standard cold dark matter (ΛCDM) cosmology. Methods. In X-rays, we analysed the XMM-Newton data available, fit a β-model, and subtracted it to identify residuals. We used Chandra data, when available, to identify point sources. In the optical, we applied a Serna & Gerbal (SG) analysis to clusters with at least 15 spectroscopic galaxy redshifts available in the cluster range. We discuss the substructure detection efficiencies of both methods.Results. XMM-Newton data were available for 32 clusters, for which we derive the X-ray luminosity and a global X-ray temperature for 25 of them. For 23 clusters we were able to fit the X-ray emissivity with a β-model and subtract it to detect substructures in the X-ray gas. A dynamical analysis based on the SG method was applied to the clusters having at least 15 spectroscopic galaxy redshifts in the cluster range: 18 X-ray clusters and 11 clusters with no X-ray data. The choice of a minimum number of 15 redshifts implies that only major substructures will be detected. Ten substructures were detected both in X-rays and by the SG method. Most of the substructures detected both in X-rays and with the SG method are probably at their first cluster pericentre approach and are relatively recent infalls. We also find hints of a decreasing X-ray gas density profile core radius with redshift. Conclusions. The percentage of mass included in substructures was found to be roughly constant with redshift values of 5-15%, in agreement both with the general CDM framework and with the results of numerical simulations. Galaxies in substructures show the same general behaviour as regular cluster galaxies; however, in substructures, there is a deficiency of both late type and old stellar population galaxies. Late type galaxies with recent bursts of star formation seem to be missing in the substructures close to the bottom of the host cluster potential well. However, our sample would need to be increased to allow a more robust analysis.

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