scholarly journals THE MASS DISTRIBUTION AND ASSEMBLY OF THE MILKY WAY FROM THE PROPERTIES OF THE MAGELLANIC CLOUDS

2011 ◽  
Vol 743 (1) ◽  
pp. 40 ◽  
Author(s):  
Michael T. Busha ◽  
Philip J. Marshall ◽  
Risa H. Wechsler ◽  
Anatoly Klypin ◽  
Joel Primack
Keyword(s):  
Mass Distribution ◽  
Milky Way ◽  
Magellanic Clouds

scholarly journals The effect of the Magellanic Clouds on the mass distribution in the galaxy

1991 ◽  
Vol 148 ◽  
pp. 487-488
Author(s):  
G. X. Song
Keyword(s):  
Mass Distribution ◽  
Milky Way ◽  
Galactic Disk ◽  
Initial Position ◽  
Tidal Effect ◽  
Magellanic Clouds ◽  
The Galaxy

The disk of the Milky Way suffered from the tidal effect as the Magellanic Clouds were passing by. Numerical stimulations were performed to study the evolution of the mass distribution in this disk. These simulations were run with the galactic disk initially flat, and different sets of the initial position and velocity of the Magellanic Clouds were considered. One of the most conspicuous observational facts is the warp of the disk of the Milky Way. Results show that the characteristics of this warp are related to the orbit of the Magellanic Clouds.

scholarly journals Life Cycle of Dust in the Magellanic Clouds and the Milky Way

2014 ◽  
Author(s):  
Svitlana Zhukovska ◽  
Thomas Henning
Keyword(s):  
Life Cycle ◽  
Milky Way ◽  
Magellanic Clouds

The Mass Distribution of the Milky Way Deduced from Globular Cluster Dynamics

1996 ◽  
pp. 697-702 ◽  
Author(s):  
B. Dauphole ◽  
J. Colin ◽  
M. Geffert ◽  
M. Odenkirchen ◽  
H.-J. Tucholke
Keyword(s):  
Mass Distribution ◽  
Globular Cluster ◽  
Milky Way

scholarly journals The interstellar medium of the Magellanic Clouds from absorption lines

1991 ◽  
Vol 148 ◽  
pp. 401-406 ◽  
Author(s):  
Klaas S. De Boer
Keyword(s):  
Interstellar Medium ◽  
Absorption Line ◽  
Milky Way ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Absorption Lines ◽  
Small Magellanic Cloud ◽  
General Aspects

General aspects of ISM studies using absorption line studies are given and available data are reviewed. Topics are: galactic foreground gas, individual fields in the Magellanic Clouds (MCs) and MC coronae. Overall investigations are discussed. It is demonstrated that the metals in the gas of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are a factor of 3 and 10, respectively, in abundance below solar levels. The depletion pattern in the LMC is similar to that of the Milky Way.

scholarly journals Interstellar Phases in the Magellanic Clouds

1999 ◽  
Vol 190 ◽  
pp. 45-50 ◽  
Author(s):  
John M. Dickey ◽  
Monika Marx-Zimmer ◽  
Christian Düsterberg ◽  
Ulrich Mebold ◽  
Snezana Stanimirović ◽  
...  
Keyword(s):  
Heavy Element ◽  
Milky Way ◽  
Magellanic Clouds ◽  
Element Abundances ◽  
Lower Abundance ◽  
Cloud Temperature ◽  
Magellanic System

Surveys of λ21-cm absorption in the Magellanic System show that the cool phase of the HI is less abundant in the SMC than in the Milky Way, and may be so also in the LMC. The typical cool cloud temperature is colder than in the Milky Way, 30 to 40 K rather than 60 to 75 K. The lower abundance of cool phase HI can be traced to the lower heavy element abundances in the Magellanic environment. The cooler cloud temperatures are somewhat mysterious.

scholarly journals The search for multiple populations in Magellanic Clouds clusters – V. Correlation between cluster age and abundance spreads

2019 ◽  
Vol 487 (4) ◽  
pp. 5324-5334 ◽  
Author(s):  
S Martocchia ◽  
E Dalessandro ◽  
C Lardo ◽  
I Cabrera-Ziri ◽  
N Bastian ◽  
...  
Keyword(s):  
Significant Role ◽  
Massive Star ◽  
Milky Way ◽  
Star Clusters ◽  
Magellanic Clouds ◽  
Key Factors ◽  
Strong Function ◽  
Combining Data ◽  
Chemical Anomalies ◽  
Cluster Age

ABSTRACT In our HST photometric survey, we have been searching for multiple stellar populations (MPs) in Magellanic Clouds (MCs) massive star clusters which span a significant range of ages (∼1.5–11 Gyr). In the previous papers of the series, we have shown that the age of the cluster represents one of the key factors in shaping the origin of the chemical anomalies. Here, we present the analysis of four additional clusters in the MCs, namely Lindsay 38, Lindsay 113, NGC 2121, and NGC 2155, for which we recently obtained new UV HST observations. These clusters are more massive than ∼104 M⊙ and have ages between ∼2.5 and ∼6 Gyr, i.e. located in a previously unexplored region of the cluster age/mass diagram. We found chemical anomalies, in the form of N spreads, in three out of four clusters in the sample, namely in NGC 2121, NGC 2155, and Lindsay 113. By combining data from our survey and HST photometry for three additional clusters in the Milky Way (namely 47 Tuc, M15, and NGC 2419), we show that the extent of the MPs in the form of N spread is a strong function of age, with older clusters having larger N spreads with respect to the younger ones. Hence, we confirm that cluster age plays a significant role in the onset of MPs.

29. Stellar Spectra (Spectres Stellaires)

1991 ◽  
Vol 21 (1) ◽  
pp. 309-326
Keyword(s):  
Milky Way ◽  
Massive Stars ◽  
Magellanic Clouds ◽  
Dynamical Interaction ◽  
Stellar Spectra ◽  
Luminous Blue Variables ◽  
Classical Novae ◽  
Giant Stars ◽  
Red Giant ◽  
Sydney Australia

In the triennium under review, from the late second half of 1987 to the early second half of 1990, Commission 29 has sponsored or cosponsored the following IAU Conferences: Coll. No. 106, “Evolution of Peculiar Red Giant Stars,” Bloomington, Indiana, July 1988; CoU. No. 114, “White Dwarfs,” Hanover, New Hamsphire, August 1988; Coll. No. 113, “Physics of Luminous Blue Variables,” Val Morin, Quebec, August 1988; Coll. No. 122, “Physics of Classical Novae,” Madrid, Spain, June 1989; Symp. No. 143, “Wolf-Rayet Stars and Interrelations with Other Massive Stars in Galaxies,” Denpasar, Indonesia, June 1990; Symp. No 148, “The Magellanic Clouds and their Dynamical Interaction with the Milky Way,” Sydney, Australia, July 1990; Symp. No. 145, “Evolution of Stars: the Photospheric Abundance Connection,” Druzba, Bulgaria. August 1990.

scholarly journals A Laboratory of Stellar Nuleosynthesis: Isotope Ratios in the Magellanic Clouds

1999 ◽  
Vol 190 ◽  
pp. 279-281 ◽  
Author(s):  
Yi-nan Chin
Keyword(s):  
Radio Astronomy ◽  
Milky Way ◽  
Isotope Ratios ◽  
Magellanic Clouds ◽  
Isotopic Species ◽  
Central Regions ◽  
Different Parts

In radio astronomy, interstellar isotope ratios have been measured for more than two decades towards different parts of the Milky Way and central regions of some star-burst galaxies. While signals are often too weak to detect rare isotopic species in relatively distant extragalactic sources, our Galaxy only provides an environment with limited metallicity range. Obviously, this constraint can be removed by observing isotopic species in the Magellanic Clouds, located only 50–60 kpc away from us. We thus observed isotope ratios of hydrogen, carbon, nitrogen, oxygen, and sulfur and the results are given in Table 1.

scholarly journals Circumstellar emission in Be/X-ray binaries of the Magellanic Clouds and the Milky Way

2012 ◽  
Vol 539 ◽  
pp. A114 ◽  
Author(s):  
M. S. Riquelme ◽  
J. M. Torrejón ◽  
I. Negueruela
Keyword(s):  
Milky Way ◽  
Magellanic Clouds ◽  
X Ray ◽  
X Ray Binaries
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