PMaC's green queue: a framework for selecting energy optimal DVFS configurations in large scale MPI applications

2013 ◽  
Vol 28 (2) ◽  
pp. 211-231 ◽  
Author(s):  
Joshua Peraza ◽  
Ananta Tiwari ◽  
Michael Laurenzano ◽  
Laura Carrington ◽  
Allan Snavely
Keyword(s):  
Large Scale ◽  
Mpi Applications

scholarly journals Power-aware load balancing of large scale MPI applications

2009 ◽  
Author(s):  
Maja Etinski ◽  
Julita Corbalan ◽  
Jesus Labarta ◽  
Mateo Valero ◽  
Alex Veidenbaum
Keyword(s):  
Load Balancing ◽  
Large Scale ◽  
Mpi Applications

scholarly journals Countdown Slack: A Run-Time Library to Reduce Energy Footprint in Large-Scale MPI Applications

2020 ◽  
Vol 31 (11) ◽  
pp. 2696-2709 ◽  
Author(s):  
Daniele Cesarini ◽  
Andrea Bartolini ◽  
Andrea Borghesi ◽  
Carlo Cavazzoni ◽  
Mathieu Luisier ◽  
...  
Keyword(s):  
Large Scale ◽  
Energy Footprint ◽  
Run Time ◽  
Mpi Applications

Some comments about observations and image processing of comet 29P/Schwassmann-Wachmann 1

1999 ◽  
Vol 173 ◽  
pp. 243-248
Author(s):  
D. Kubáček ◽  
A. Galád ◽  
A. Pravda
Keyword(s):  
Image Processing ◽  
Large Scale ◽  
Harvard College ◽  
Oak Ridge ◽  
Large Scale Structures ◽  
Short Period Comet ◽  
Short Period ◽  
Scale Structures ◽  
Harvard College Observatory ◽  
Period Comet

AbstractUnusual short-period comet 29P/Schwassmann-Wachmann 1 inspired many observers to explain its unpredictable outbursts. In this paper large scale structures and features from the inner part of the coma in time periods around outbursts are studied. CCD images were taken at Whipple Observatory, Mt. Hopkins, in 1989 and at Astronomical Observatory, Modra, from 1995 to 1998. Photographic plates of the comet were taken at Harvard College Observatory, Oak Ridge, from 1974 to 1982. The latter were digitized at first to apply the same techniques of image processing for optimizing the visibility of features in the coma during outbursts. Outbursts and coma structures show various shapes.

Evolution of Large-Scale Coronal Structures

1994 ◽  
Vol 144 ◽  
pp. 29-33
Author(s):  
P. Ambrož
Keyword(s):  
Magnetic Field ◽  
Field Line ◽  
Large Scale ◽  
Coronal Magnetic Field ◽  
Source Surface ◽  
Solar Cycles ◽  
Characteristic Relationship ◽  
The Magnetic Field ◽  
Coronal Structures

AbstractThe large-scale coronal structures observed during the sporadically visible solar eclipses were compared with the numerically extrapolated field-line structures of coronal magnetic field. A characteristic relationship between the observed structures of coronal plasma and the magnetic field line configurations was determined. The long-term evolution of large scale coronal structures inferred from photospheric magnetic observations in the course of 11- and 22-year solar cycles is described.Some known parameters, such as the source surface radius, or coronal rotation rate are discussed and actually interpreted. A relation between the large-scale photospheric magnetic field evolution and the coronal structure rearrangement is demonstrated.

Large-scale Motion of Solar Filaments

2000 ◽  
Vol 179 ◽  
pp. 205-208
Author(s):  
Pavel Ambrož ◽  
Alfred Schroll
Keyword(s):  
Magnetic Flux ◽  
Proper Motion ◽  
Time Scale ◽  
Large Scale ◽  
Accuracy Of Measurements ◽  
Solar Filaments ◽  
General Movement ◽  
Scale Motion ◽  
Velocity Scatter

AbstractPrecise measurements of heliographic position of solar filaments were used for determination of the proper motion of solar filaments on the time-scale of days. The filaments have a tendency to make a shaking or waving of the external structure and to make a general movement of whole filament body, coinciding with the transport of the magnetic flux in the photosphere. The velocity scatter of individual measured points is about one order higher than the accuracy of measurements.

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