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Hensler, G.; Tschöke, D.; Bomans, D. J.; Boselli, A.

doi:10.1023/a:1024091824291

Cited by 3 publications

(8 citation statements)

References 10 publications

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“…NGC 4569 has smooth, relatively featureless, outer spiral arms and a ring of star formation at 0.3 r 24 . A distinct peculiar arm of HII regions, which begins at the Hα truncation radius and has an HI counterpart , may be extraplanar (Hensler et al 2003). This arm resembles the one-arm gas morphologies commonly seen in the ICM-ISM interaction simulations of Schulz & Struck (2001) and Vollmer et al (2001).…”

Section: Truncated Spirals With Normal Inner Disksmentioning

confidence: 70%

“…Simulations including the effects of rotation on ICM-ISM interactions show in some phases one dominant extraplanar gas arm emerging from the outer edges of truncated gas disk (Vollmer et al 2001;Schulz & Struck 2001). Such arms may be observed in NGC 4548 (Vollmer et al 2000), NGC 4654 (Phookun & Mundy 1995;Vollmer 2003), and NGC 4569 Hensler et al 2003;Kenney et al in prep). Simulations show that the arms can transfer angular momentum from the inner gas disk, which can make a contracted, denser, 'annealed' inner gas disk, which has some resistance to further stripping (Schulz & Struck 2001).…”

Section: Icm-ism Interactionsmentioning

confidence: 98%

“…6.-Three Virgo Cluster galaxies with star forming disks truncated within 0.4r 24 , normal-enhanced inner star formation rates, and peculiar Hα distributions, possibly extraplanar emission. NGC 4569 has a ring of star formation at about 0.3r 24 and a detached arm of HII regions, which may be extraplanar (Hensler et al 2003). NGC 4522 appears to interacting with the ICM, based on the extraplanar HII regions and disturbed HI and radio continuum (Kenney & Koopmann 1999;Kenney et al 2004) The Hα emission in NGC 4351 is offset from the apparent center in R. See Figure 4 for details on the plots.…”

Section: Truncated Spirals With Enhanced Total Starmentioning

confidence: 99%

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Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies

Koopmann

Kenney

2004

ApJ

285

348

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We describe the various Hα morphologies of Virgo Cluster and isolated spiral galaxies, and associate the Hα morphologies with the types of environmental interactions which have altered the cluster galaxies. The spatial distributions of Hα and R-band emission are used to divide the star formation morphologies of the 52 Virgo Cluster spirals into several categories: normal (37%), anemic (6%), enhanced (6%), and (spatially) truncated (52%). Truncated galaxies are further subdivided based on their inner star formation rates into truncated/normal (37%), truncated/compact (6%), truncated/anemic (8%), and truncated/enhanced (2%). The fraction of anemic galaxies is relatively small (6-13%) in both environments, suggesting that starvation is not a major factor in the reduced star formation rates of Virgo spirals. The majority of Virgo spiral galaxies have their Hα disks truncated (52%), whereas truncated Hα disks are rarer in isolated galaxies (12%). Most of the Hα-truncated galaxies have relatively undisturbed stellar disks and normal-to-slightly enhanced inner disk star formation rates, suggesting that ICM-ISM stripping is the main mechanism causing the reduced star formation rates of Virgo spirals. Several of the truncated galaxies are peculiar, with enhanced central star formation rates, disturbed stellar disks, and bar-like distributions of luminous HII complexes inside the central 1 kpc, but no star formation beyond, suggesting recent tidal interactions or minor mergers have also influenced their morphology. Two highly-inclined Hα-truncated spirals have numerous extraplanar HII regions, and are likely in an active phase of ICM-ISM stripping. Several spirals have one-sided Hα enhancements at the outer edge of their truncated Hα disks, suggesting modest and local enhancements in their star formation rates due to ICM-ISM interactions. Low-velocity tidal interactions and perhaps outer cluster HI accretion seem to be the triggers for enhanced global star formation in four Virgo galaxies. These results indicate that most Virgo spiral galaxies experience ICM-ISM stripping, many experience significant tidal effects, and many experience both.

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Section: Truncated Spirals With Normal Inner Disksmentioning

confidence: 70%

Section: Icm-ism Interactionsmentioning

confidence: 98%

Section: Truncated Spirals With Enhanced Total Starmentioning

confidence: 99%

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Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies

Koopmann

Kenney

2004

ApJ

285

348

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“…From a literature search, we summarize as follows the characteristics of spectral lines of HD 175362 and their phase relation with the photometric and magnetic field data. Balona (1975), Wolff & Wolff (1976), Hensler (1979) and Catalano & Leone (1996) report that the Si II line strengths vary in antiphase with helium, that the velocity variations are in quadrature with the variations of line strength, and that the light curves are in antiphase with respect to the He line strength. This does not seem to be incompatible with a pulsation model (De Ridder 2001).…”

Section: Geneva Photometrymentioning

confidence: 98%

“…In the literature, the variablitity of HD 175362 is interpreted in terms of the oblique rotator model. For instance, Hensler (1979) modelled the star with a single He-cap and a single Si-cap located at the opposite magnetic poles.…”

Section: Geneva Photometrymentioning

confidence: 99%

On the co-existence of chemically peculiar Bp stars, slowly pulsating B stars and constant B stars in the same part of the HR diagram

Briquet¹,

Hubrig

Cat

et al. 2007

A&A

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Aims. In order to better model massive B-type stars, we need to understand the physical processes taking place in slowly pulsating B (SPB) stars, chemically peculiar Bp stars, and non-pulsating normal B stars co-existing in the same part of the H-R diagram. Methods. We carry out a comparative study between samples of confirmed and well-studied SPB stars and a sample of well-studied Bp stars with known periods and magnetic field strengths. We determine their evolutionary state using accurate HIPPARCOS parallaxes and Geneva photometry. We discuss the occurrence and strengths of magnetic fields as well as the occurrence of stellar pulsation among both groups. Further, we make a comparison of Geneva photometric variability for both kinds of stars.Results. The group of Bp stars is significantly younger than the group of SPB stars. Longitudinal magnetic fields in SPB stars are weaker than those of Bp stars, suggesting that the magnetic field strength is an important factor for B type stars to become chemically peculiar. The strongest magnetic fields appear in young Bp stars, indicating a magnetic field decay in stars at advanced ages. Rotation periods of Bp and pulsation periods of SPB stars are of the same order and the behaviour of Geneva photometric variability of some Bp stars cannot be distinguished from the variability of SPB stars, illustrating the difficulty to interpret the observed variability of the order of days for B-type stars. We consider the possibility that pulsation could be responsible for the variability among chemically peculiar stars. In particular, we show that a non-linear pulsation model is not excluded by photometry for the Bp star HD 175362.

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Digital Justice

Rabinovich‐Einy¹,

Katsh²

2014

International Journal of Online Dispute Resolution

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Digital technology is transforming the landscape of dispute resolution: it is generating an ever growing number of disputes and at the same time is challenging the effectiveness and reach of traditional dispute resolution avenues. While technology has been a disruptive force in the field, it also holds a promise for an improved dispute resolution landscape, one that is based on fewer physical, conceptual, psychological and professional boundaries, while enjoying a higher degree of transparency, participation and change. This promise remains to be realized as the underlying assumptions and logic of the field of dispute resolution have remained as they were since the last quarter of the 20th century, failing to reflect the future direction dispute resolution mechanisms can be expected to follow, as can be learned from the growth of online dispute resolution. This article explores the logic of boundaries that has shaped the traditional dispute resolution landscape, as well as the challenges such logic is facing with the spread of online dispute resolution.

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Untitled

Cited by 3 publications

References 10 publications

Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies

Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies

On the co-existence of chemically peculiar Bp stars, slowly pulsating B stars and constant B stars in the same part of the HR diagram

Digital Justice

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