scholarly journals g -mode oscillations in hybrid stars: A tale of two sounds

2021 ◽  
Vol 103 (12) ◽  
Author(s):  
Prashanth Jaikumar ◽  
Alexandra Semposki ◽  
Madappa Prakash ◽  
Constantinos Constantinou
Keyword(s):  
Hybrid Stars

Discontinuity g ‐modes of hybrid stars: Effect of sequential phase transitions

2021 ◽  
Author(s):  
Maria Camila Rodríguez ◽  
Ignacio F. Ranea‐Sandoval ◽  
Mauro Mariani ◽  
Germán Malfatti ◽  
Octavio Miguel Guilera
Keyword(s):  
Phase Transitions ◽  
Hybrid Stars ◽  
Sequential Phase

scholarly journals Rotating hybrid stars with the Dyson-Schwinger quark model

2017 ◽  
Vol 96 (4) ◽  
Author(s):  
J.-B. Wei ◽  
H. Chen ◽  
G. F. Burgio ◽  
H.-J. Schulze
Keyword(s):  
Quark Model ◽  
Hybrid Stars

Influence of medium effects on the rotating hybrid stars

2010 ◽  
Vol 34 (11) ◽  
pp. 1696-1699
Author(s):  
Miao Kang ◽  
Xia Zhou ◽  
Xiao-Dong Wang ◽  
Yao-Fu Heng
Keyword(s):  
Medium Effects ◽  
Hybrid Stars

Hybrid stars

Pramana ◽  
2004 ◽  
Vol 62 (3) ◽  
pp. 753-756 ◽  
Author(s):  
Ashok Goyal
Keyword(s):  
Hybrid Stars

scholarly journals Implementation of the Nambu Jona-Lasinio model in hybrid stars

2010 ◽  
Vol 525 ◽  
pp. L1 ◽  
Author(s):  
O. Benhar ◽  
A. Cipollone
Keyword(s):  
Hybrid Stars

scholarly journals Chromospheric variation in cool supergiant stars

1996 ◽  
Vol 176 ◽  
pp. 415-422
Author(s):  
J. A. Eaton ◽  
G. W. Henry
Keyword(s):  
Main Sequence ◽  
Active Regions ◽  
Magnetic Activity ◽  
Hybrid Stars ◽  
Magnetic Phenomena ◽  
Dividing Line

Stars close to the main sequence, if they rotate rapidly enough, show magnetic activity in the form of spots, active regions, and strong chromospheres. With the exception of the hybrid stars, stars cooler and more luminous than the so-called Linsky-Haisch dividing line, in contrast, are not known to have any of these phenomena. In fact, it is not clear such stars, even though rotating and convective, show any magnetic phenomena at all. We discuss (1) photometry used to search for spots in the hybrid stars, which we have not found, and (2) evidence for chromospheric variation in K supergiants that takes the form of enhanced winds, but which may be analogous to the activity of stars closer to the main sequence.

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