scholarly journals A Companion Star Launching Jets in the Wind Acceleration Zone of a Giant Star

2020 ◽  
Vol 891 (1) ◽  
pp. 33 ◽  
Author(s):  
Shlomi Hillel ◽  
Ron Schreier ◽  
Noam Soker
Keyword(s):  
Giant Star ◽  
Companion Star ◽  
Acceleration Zone

scholarly journals A Statistical Study of Spectroscopic Binaries Containing A Late-Type Giant Star

1989 ◽  
Vol 106 ◽  
pp. 222-222
Author(s):  
H.M.J. Boffin
Keyword(s):  
Mass Transfer ◽  
Statistical Study ◽  
Asymptotic Giant Branch ◽  
Spectroscopic Binaries ◽  
Red Giants ◽  
Late Type ◽  
Giant Star ◽  
Companion Star ◽  
Observational Fact ◽  
Type Giant

Binarity seems to be a feature shared by various classes of Peculiar Red Giants (PRG). This observational fact has led to the general agreement that those stars result from a mass transfer originating from an asymptotic giant branch companion star.

Far infrared study of the giant star forming complex W 51

2002 ◽  
Vol 4 ◽  
pp. 333-333
Author(s):  
S. K. Ghosh ◽  
D. K. Ojha ◽  
R. P. Verma
Keyword(s):  
Far Infrared ◽  
Infrared Study ◽  
Giant Star ◽  
Star Forming

scholarly journals The giant star forming halo associated with the radio galaxy PKS 1932-46

2005 ◽  
Vol 359 (1) ◽  
pp. L5-L9 ◽  
Author(s):  
M. Villar-Martin ◽  
C. Tadhunter ◽  
R. Morganti ◽  
J. Holt
Keyword(s):  
Radio Galaxy ◽  
Giant Star ◽  
Star Forming

scholarly journals Detection of a planetary companion around the giant star γ1Leonis

2010 ◽  
Vol 509 ◽  
pp. A24 ◽  
Author(s):  
Inwoo Han ◽  
B. C. Lee ◽  
K. M. Kim ◽  
D. E. Mkrtichian ◽  
A. P. Hatzes ◽  
...  
Keyword(s):  
Giant Star

scholarly journals The nature of the companion star in Circinus X-1

2015 ◽  
Vol 456 (1) ◽  
pp. 347-355 ◽  
Author(s):  
Helen M. Johnston ◽  
Roberto Soria ◽  
Joel Gibson
Keyword(s):  
Companion Star

Magnetised Wave Collapse in Solar System Plasmas

1993 ◽  
Vol 10 (4) ◽  
pp. 283-286 ◽  
Author(s):  
Andrew Melatos ◽  
Peter Robinson
Keyword(s):  
Solar System ◽  
Wave Packets ◽  
Particle Interactions ◽  
Coherent Wave ◽  
Wave Collapse ◽  
Non Linear ◽  
Acceleration Zone ◽  
The Waves ◽  
Linear Plasma

AbstractClumpy, intense wave packets observed in situ in the Jovian and terrestrial electron foreshocks, and in the Earth’s auroral acceleration zone, point to the existence of non-linear plasma turbulence in these regions. In non-linear turbulence, wave packets collapse to short scales and high fields, stopping only when coherent wave-particle interactions efficiently dissipate the energy in the waves. The purpose of this paper is to examine the shortest scales and highest fields achieved during collapse in a strongly magnetised plasma, and identify parts of the solar system where the magnetised aspects of wave collapse are important.

Additional players and half-court areas enhance group tactical-technical behavior and decrease physical and physiological responses in basketball small-sided games

2021 ◽  
pp. 174795412110536
Author(s):  
Sarah da Glória Teles Bredt ◽  
Daniel de Souza Camargo ◽  
Bernardo Vidigal Borges Mortoza ◽  
André Gustavo Pereira de Andrade ◽  
Leopoldo Augusto Paolucci ◽  
...  
Keyword(s):  
Heart Rate ◽  
Physiological Responses ◽  
Team Sports ◽  
Male Athletes ◽  
Heart Rate Monitors ◽  
Numerical Equality ◽  
Acceleration Zone ◽  
Physical Performances ◽  
Number Of Passes ◽  
Game Type

Small-sided games are used to improve tactical-technical and physical performances in team sports. This study compared the physical, physiological, and tactical-technical responses during 3 versus 3 basketball small-sided games performed in full and half-court: numerical equality (3 vs. 3), numerical superiority (4 vs. 3), and with a non-scorer floater (3 vs. 3  +  1). A total of 45 U-14 and U-15 male athletes participated in the study. They were divided into three-player teams and played one 4-minute bout of each small-sided game type. Heart rate and the time spent in four acceleration zones (0.0–0.5, 0.5–1.0, 1.0–1.5, and 1.5–2.0 g) were recorded using heart rate monitors and triaxial accelerometers. Small-sided games were filmed for the analysis of tactical-technical behavior. Results showed a higher frequency of space creation without the ball, and a mean number of passes per offense in the formats 4 versus 3 and 3 versus 3  +  1, and a lower frequency of space creation with the ball dribbled in 3 versus 3  +  1 compared with 3 versus 3. Physical and physiological responses were higher in the full-court regardless of format and in numerical equality regardless of court area; only the time spent in the highest acceleration zone was higher in half-court small-sided games. We concluded that additional players increase group tactical actions and decrease physical and physiological responses in 3 versus 3 basketball small-sided games.

scholarly journals K2-97b: A (RE-?)INFLATED PLANET ORBITING A RED GIANT STAR

2016 ◽  
Vol 152 (6) ◽  
pp. 185 ◽  
Author(s):  
Samuel K. Grunblatt ◽  
Daniel Huber ◽  
Eric J. Gaidos ◽  
Eric D. Lopez ◽  
Benjamin J. Fulton ◽  
...  
Keyword(s):  
Giant Star ◽  
Red Giant

scholarly journals Eclipsing spotted giant star with K2 and historical photometry

2018 ◽  
Vol 620 ◽  
pp. A189 ◽  
Author(s):  
K. Oláh ◽  
S. Rappaport ◽  
T. Borkovits ◽  
T. Jacobs ◽  
D. Latham ◽  
...  
Keyword(s):  
Binary System ◽  
Main Sequence ◽  
Rapid Evolution ◽  
Magnetic Activity ◽  
Primary Component ◽  
Physical Parameters ◽  
Giant Star ◽  
Eclipsing Binary ◽  
Giant Stars ◽  
Active Stars

Context. Stars can maintain their observable magnetic activity from the pre-main sequence (PMS) to the tip of the red giant branch. However, the number of known active giants is much lower than active stars on the main sequence (MS) since the stars spend only about 10% of their MS lifetime on the giant branch. Due to their rapid evolution it is difficult to estimate the stellar parameters of giant stars. A possibility for obtaining more reliable stellar parameters for an active giant arises when it is a member of an eclipsing binary system. Aims. We have discovered EPIC 211759736, an active spotted giant star in an eclipsing binary system during the Kepler K2 Campaign 5. The eclipsing nature allows us to much better constrain the stellar parameters than in most cases of active giant stars. Methods. We have combined the K2 data with archival HATNet, ASAS, and DASCH photometry, new spectroscopic radial velocity measurements, and a set of follow-up ground-based BVRCIC photometric observations, to find the binary system parameters as well as robust spot models for the giant at two different epochs. Results. We determined the physical parameters of both stellar components and provide a description of the rotational and long-term activity of the primary component. The temperatures and luminosities of both components were examined in the context of the Hertzsprung–Russell diagram. We find that both the primary and the secondary components deviate from the evolutionary tracks corresponding to their masses in the sense that the stars appear in the diagram at lower masses than their true masses. Conclusions. We further evaluate the proposition that traditional methods generally result in higher masses for active giants than what is indicated by stellar evolution tracks in the HR diagram. A possible reason for this discrepancy could be a strong magnetic field, since we see greater differences in more active stars.

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