Slavkov u Brna

Kroupa, Jiří

doi:10.1093/gao/9781884446054.article.t079169

Cited by 3 publications

(4 citation statements)

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“…The total masses of the LMC and the SMC are 1.0 × 10 10 M ⊙ and 3.0 × 10 9 M ⊙ , respectively. These values were based on those derived from the latest observations (e.g., Kroupa & Bastian 1997;van der Marel et al 2002) and consistent with previous simulations (e.g., Gardiner & Noguchi 1996). In the Clouds' orbital calculations with the backward integration scheme (Gardiner et al 1994), we assume that the current space velocities (V x , V y , V z ) (or (U, V, W )) in units of km s −1 are (−5, −225, 194) and (40, −185, 171).…”

Section: Discussionsupporting

confidence: 87%

Explaining the Mysterious Age Gap of Globular Clusters in the Large Magellanic Cloud

Bekki

Couch

Beasley

et al. 2004

ApJ

101

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The Large Magellanic Cloud (LMC) has a unique cluster formation history in that nearly all of its globular clusters were formed either ∼ 13 Gyr ago or less than ∼ 3 Gyr ago. It is not clear what physical mechanism is responsible for the most recent cluster formation episode and thus the mysterious age gap between the LMC clusters. We first present results of gas dynamical N-body simulations of the evolution of the LMC in the context of its Galactic orbit and interactions with the SMC, paying special attention to the effect of tidal forces. We find that the first close encounter between the LMC and the Small Magellanic Cloud (SMC) about 4 Gyr ago was the beginning of a period of strong tidal interaction which likely induced dramatic gas cloud collisions, leading to an enhancement of the formation of globular clusters which has been sustained by strong tidal interactions to the present day. The tidal interaction results in the formation of a barred, elliptical, thick disk in the LMC. The model also predicts the presence of a large, diffuse stellar stream circling the Galaxy, which originated from the LMC.

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Section: Discussionsupporting

confidence: 87%

Explaining the Mysterious Age Gap of Globular Clusters in the Large Magellanic Cloud

Bekki

Couch

Beasley

et al. 2004

ApJ

101

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“…We base the parameter values of the LMC/SMC orbital properties on the early numerical simulations of Gardiner & Noguchi (1996), which are not only consistent with the observed location and radial velocity of the LMC/SMC system but are also successful in reproducing the observed physical properties of the Magellanic stream. The orbital parameters in the present study (and thus in Gardiner & Noguchi 1996) are broadly consistent with the Hipparcos data of Kroupa & Bastian (1997), as shown by Yoshizawa & Noguchi (2003). Therefore, the adopted parameter values can be regarded as reasonable, although the exact orbital properties of the LMC/SMC system have not been observationally determined (thus, the orbital parameters should be still free parameters).…”

Section: Tidal Interaction In the Lmc/smc Systemsupporting

confidence: 87%

Formation of Star Clusters in the Large Magellanic Cloud and Small Magellanic Cloud. I. Preliminary Results on Cluster Formation from Colliding Gas Clouds

Bekki

Beasley

Forbes

et al. 2004

ApJ

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We demonstrate that single and binary star clusters can be formed during cloud-cloud collisions triggered by the tidal interaction between the Large and Small Magellanic clouds. We run two different sets of self-consistent numerical simulations that show that compact, bound star clusters can be formed within the centers of two colliding clouds as a result of strong gaseous shocks, compression, and dissipation, provided that the clouds have moderately large relative velocities (10-60 km s À1 ). The impact parameter determines whether the two colliding clouds become a single or a binary cluster. The star formation efficiency in the colliding clouds is dependent on the initial ratio of the relative velocity of the clouds to the sound speed of the gas. Based on these results, we discuss the observed larger fraction of binary clusters, and star clusters with high ellipticity, in the Magellanic clouds.

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“…We calculated the ASPF for the LMC using the Jones et al (1994) proper motion, however their reduction of this proper motion to an absolute reference frame was complicated by the unknown amount of rotation of the stars around the center of the LMC. If we instead calculate the ASPF using the Jones et al (1994) LMC proper motion corrected for the estimated amount of rotation in the field or with the Kroupa & Bastian (1997) LMC proper motion, we find that the ASPF in either of these cases lies almost entirely in the northern Galactic hemisphere, indicating that for the LMC, L z is positive, and opposite that of the SMC and Ursa Minor. However, since these objects are all on nearly polar orbits and are in the outer halo where the potential is more nearly spherical, the difference in the sign of L z may not be meaningful.…”

Section: Dynamical Groupsmentioning

confidence: 76%

“…We have followed the recommendation of Dinescu et al (1999b) on the proper motion of NGC 362 and adopt the Tucholke (1992b) proper motion of this object, which is calculated relative to SMC stars. However, Dinescu et al (1999b) derives an absolute proper motion for NGC 362 by correcting for the SMC's proper motion using the Kroupa & Bastian (1997) measurement. The corrected ASPF has a center more than 50 • from the center of the uncorrected proper motion's pole family.…”

Section: Pole Families From Independent Proper Motion Measurementsmentioning

confidence: 99%

On the Distribution of Orbital Poles of Milky Way Satellites

Palma

Majewski

Johnston

2002

ApJ

147

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In numerous studies of the outer Galactic halo some evidence for accretion has been found. If the outer halo did form in part or wholly through merger events, we might expect to find coherent streams of stars and globular clusters following similar orbits as their parent objects, which are assumed to be present or former Milky Way dwarf satellite galaxies. We present a study of this phenomenon by assessing the likelihood of potential descendant ``dynamical families'' in the outer halo. We conduct two analyses: one that involves a statistical analysis of the spatial distribution of all known Galactic dwarf satellite galaxies (DSGs) and globular clusters, and a second, more specific analysis of those globular clusters and DSGs for which full phase space dynamical data exist. In both cases our methodology is appropriate only to members of descendant dynamical families that retain nearly aligned orbital poles today. Since the Sagittarius dwarf (Sgr) is considered a paradigm for the type of merger/tidal interaction event for which we are searching, we also undertake a case study of the Sgr system and identify several globular clusters that may be members of its extended dynamical family. (ABRIDGED)Comment: accepted by ApJ, 57 pages, 13 figures, AASTeX forma

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Slavkov u Brna

Cited by 3 publications

References 0 publications

Explaining the Mysterious Age Gap of Globular Clusters in the Large Magellanic Cloud

Explaining the Mysterious Age Gap of Globular Clusters in the Large Magellanic Cloud

Formation of Star Clusters in the Large Magellanic Cloud and Small Magellanic Cloud. I. Preliminary Results on Cluster Formation from Colliding Gas Clouds

On the Distribution of Orbital Poles of Milky Way Satellites

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