Spin glasses in a magnetic field: Phase diagram and dynamics

Lefloch, F.; Hammann, J.; Ocio, M.; Vincent, E.

doi:10.1016/0921-4526(94)90278-x

Cited by 218 publications

(386 citation statements)

References 29 publications

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“…It is our position that they essentially formed there inside the BRC that has since retreated to its present position. Then the above fact suggests that they were formed in the (first) collapse phase of the evolution of BRCs (Lefloch, Lazareff 1994). Presumably BRCs may have a second (or, even third) collapse phase due to their clumpiness or as the exciting O star(s) evolve(s) and increase(s) its (their) UV photon emission, or somehow they give birth to stars after this phase (i.e., in the cometary phase); and the stars on or near the bright rim, which generally are younger, may correspond to such origin.…”

Section: Discussionmentioning

confidence: 99%

“…Theoretically, triggered star formation caused by the compression of the gas due to shock is expected to take place in such a pre-existing dense clump in an H II region. This phenomenon is called radiation-driven implosion (RDI) and detailed model calculations were carried out by several authors (e.g., Bertoldi 1989, Lefloch, Lazareff 1994, Miao et al 2006). Many molecular line and radio continuum observations of BRCs (Lefloch, Lazareff 1995, Lefloch, Lazareff, Castets 1997, De Vries, Narayanan, Snell 2002, Thompson et al 2004a, Thompson et al 2004b, Thompson, White 2004c, Urquhart et al 2006 show that the overall morphology and some physical properties of them are consistent with those of the RDI models.…”

Section: Introductionmentioning

confidence: 99%

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Age Sequence in Small Clusters Associated with Bright-Rimmed Clouds

Ogura

Chauhan

Pandey

et al. 2007

Publications of the Astronomical Society of Japan

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Bright-rimmed clouds (BRCs) found in H II regions are probable sites of triggered star formation due to compression by ionization/shock fronts, and it is hypothesized that star formation proceeds from the exciting star(s) side outward of the H II region ("small-scale sequential star formation"). In order to quantitatively testify this hypothesis we undertook BVI c photometry of four BRC aggregates. The amounts of interstellar extinction and reddening for each star have been estimated by using the JHK s photometry. Then we constructed reddening-corrected V/V-I c color-magnitude diagrams, where the age of each star has been derived. All the stars turned out to be a few tenths to a few Myr old. Although the scatters are large and the numbers of the sample stars are small, we found a clear trend that the stars inside or in the immediate vicinity of the bright rim are younger than those outside it in all the four aggregates, confirming the hypothesis in question.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Age Sequence in Small Clusters Associated with Bright-Rimmed Clouds

Ogura

Chauhan

Pandey

et al. 2007

Publications of the Astronomical Society of Japan

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“…The distribution of infrared emission in the WISE wavelength bands shows that the gas in S1 is hotter on the side that faces the ionizing star (figure 5). At present the S1 condensation is elongated tangentially but it is possible that eventually condensation S1 will become more elongated in the radial direction and will become a classical cometary globule (Lefloch & Lazareff 1994). The morphology of the optical and infrared emission and their spectral characteristics show that S1 represents a site of active interaction of the ionizing star emission with the dense gas clump.…”

Section: A Scenario For Star Formation In the S233 Regionmentioning

confidence: 99%

“…Another scenario for triggered star formation is contraction of a pre-existing clump due to radiation-driven implosion (Lefloch & Lazareff 1994;Kessel-Deynet & Burkert 2003;Miao et al 2006) or to a shock wave from the expanding H II region (Boss 1995). This scenario predicts a random distribution of molecular clumps around the H II region.…”

Section: A Scenario For Star Formation In the S233 Regionmentioning

confidence: 99%

Star formation in the S233 region

Ladeyschikov¹,

Соболев²,

Parfenov³

et al. 2015

Mon. Not. R. Astron. Soc.

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The main objective of this paper is to study the possibility of triggered star formation on the border of the H II region S233, which is formed by a B-star. Using high-resolution spectra we determine the spectral class of the ionizing star as B0.5 V and the radial velocity of the star to be −17.5 ± 1.4 km s −1 . This value is consistent with the velocity of gas in a wide field across the S233 region, suggesting that the ionizing star was formed from a parent cloud belonging to the S233 region. By studying spatial-kinematic structure of the molecular cloud in the S233 region, we detected an isolated clump of gas producing CO emission red-shifted relative to the parent cloud. In the UKIDSS and WISE images, the clump of gas coincides with the infrared source containing a compact object and bright-rimmed structure. The bright-rimmed structure is perpendicular to the direction of the ionizing star. The compact source coincides in position with IRAS source 05351+3549. All these features indicate a possibility of triggering formation of a next-generation star in the S233 region. Within the framework of a theoretical one-dimensional model we conclude that the 'collect-and-collapse' process is not likely to take place in the S233 region. The presence of the bright-rimmed structure and the compact infrared source suggest that the 'collapse of the pre-existing clump' process is taking place.

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“…To ascertain whether this is the case, it is necessary to compare the pressure of the ionized layer bordering the molecular cloud with the molecular pressure. If the cloud is under-pressured with respect to the ionized layer or the pressures are similar, the ionization front will be able to propagate into the cloud and then modify its evolution (Lefloch & Lazareff 1994).…”

Section: Young Stellar Populationmentioning

confidence: 99%

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

Cichowolski

Suad

Pineault

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a study of the molecular CO gas and mid/far infrared radiation arising from the environment surrounding the Wolf-Rayet (W-R) star 130. We use the multi-wavelength data to analyze the properties of the dense gas and dust, and its possible spatial correlation with that of Young Stellar Objects (YSOs). We use CO J=1-0 data from the FCRAO survey as tracer of the molecular gas, and mid/far infrared data from the recent WISE and Herschel space surveys to study the dust continuum radiation and to identify a population of associated candidate YSOs. The spatial distribution of the molecular gas shows a ring-like structure very similar to that observed in the H i gas, and over the same velocity interval. The relative spatial distribution of the H i and CO components is consistent with a photo-dissociation region. We have identified and characterized four main and distinct molecular clouds that create this structure. Cold dust is coincident with the dense gas shown in the CO measurements. We have found several cYSOs that lie along the regions with the highest gas column density, and suggest that they are spatially correlated with the shell. These are indicative of regions of star formation induced by the strong wind and ionization of the WR star.

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Spin glasses in a magnetic field: Phase diagram and dynamics

Cited by 218 publications

References 29 publications

Age Sequence in Small Clusters Associated with Bright-Rimmed Clouds

Age Sequence in Small Clusters Associated with Bright-Rimmed Clouds

Star formation in the S233 region

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

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