scholarly journals Fast ejecta resulted from jet–wind interaction in the Great Eruption of Eta Carinae

2020 ◽  
Vol 494 (3) ◽  
pp. 3186-3199
Author(s):  
Muhammad Akashi ◽  
Amit Kashi

ABSTRACT The accretion model for the 19th century Great Eruption (GE) of η Carinae suggests that mass outflowing from the primary was accreted on to the secondary, and the gravitational energy of that mass accounts for the increase in luminosity and most of the kinetic energy of the ejecta. It further argues that the accretion was accompanied by the ejection of two jets that shaped the bipolar Homunculus nebula. Observations of echos from the GE found emission lines with broad wings suggesting some of the mass in equatorial directions reached more than $10\, 000 \, \rm {km\, s^{-1}}$. We run hydrodynamic simulations following periastron passage during the GE, launching jets from the secondary as it accreted gas erupted from the primary. We then follow the interaction of the polar jets with the surrounding primary wind, as they accelerate part of the flow to velocities ${\gt}10\, 000 \, \rm {km\, s^{-1}}$ and deflect it towards lower latitudes. We find that the amount of mass that reached these high velocities during the GE is $M_h \approx 0.02 \, \rm {M_{\odot }}$. This value reaches maximum and then decreases with time. Our simulations agree with previous results of the accretion model from which we estimate Mh taking into account the energy budget of the GE. The accretion model can explain the observations of high velocity gas in light echos with the known two stars, and a triple star system is not required.

2003 ◽  
Vol 3 (S1) ◽  
pp. 349-360 ◽  
Author(s):  
Wolfgang Kundt ◽  
Christoph Hillemanns
Keyword(s):  

1997 ◽  
Vol 485 (1) ◽  
pp. 350-358 ◽  
Author(s):  
Ning Liu ◽  
Douglas R. Gies ◽  
Ying Xiong ◽  
Reed L. Riddle ◽  
William G. Bagnuolo, Jr. ◽  
...  

1997 ◽  
Vol 114 ◽  
pp. 805 ◽  
Author(s):  
B. Zuckerman ◽  
Richard A. Webb ◽  
E. E. Becklin ◽  
Ian S. McLean ◽  
Matthew A. Malkan
Keyword(s):  

1984 ◽  
Vol 80 ◽  
pp. 95-99
Author(s):  
W. C. Seitter

AbstractSpectroscopic observations through most of the eclipse cycle of BT Mon reveal the presence of both low and high velocity gas streams. Acceleration through a Laval-nozzle-effect at the inner Lagrangian point of the system and powering of the emission lines through kinetic energy losses of Coriolis deflected and subsequently colliding gas streams are considered as possible mechanisms at work in the system.


1980 ◽  
Vol 5 ◽  
pp. 517-519
Author(s):  
S. A. Colgate ◽  
A. G. Petschek

We show that Rayleigh-Taylor convective overturn of the dynamically formed lepton-trapped core of a supernova is a likely outcome of three sequential events: (1) The bounce or weak reversal shock; (2) the diffusive and convective lepton release from the neutrino-sphere during a fraction of the reversal time (≌ 100 ms); and (3) the rapid (≤ 10 ms) Rayleigh-Taylor growth of the l = 2 mode of an initial rotational perturbation. The overturn releases gravitational energy corresponding to a differential trapped lepton pressure energy of 30 to 50 MeV/nucleon by P dV work in beta equilibrium in a fraction of a millisecond. The resulting kinetic energy of ≌ 7 × 1052 ergs is more than adequate to cause the observed supernova emission. Also, the sudden release of ≌ 7 × 1051 ergs of ˜ 10 MeV neutrinos from the neutrinosphere will cause adequate mass and energy ejection.


2017 ◽  
Vol 851 (2) ◽  
pp. 132 ◽  
Author(s):  
Ian Czekala ◽  
Sean M. Andrews ◽  
Guillermo Torres ◽  
Joseph E. Rodriguez ◽  
Eric L. N. Jensen ◽  
...  

Eos ◽  
2016 ◽  
Vol 97 ◽  
Author(s):  
JoAnna Wendel
Keyword(s):  

The newly discovered planet balances precariously in orbit within the star system, puzzling scientists.


1979 ◽  
Vol 53 ◽  
pp. 43-47
Author(s):  
R. H. Durisen ◽  
J. N. Imamura

In the special case of the Maclaurin spheroids, it has been known for some time that the m = 2 barlike modes become secularly unstable for t ≡ T/IWI ≥ 0.1376 where T is the total rotational kinetic energy and W is the total gravitational energy of the spheroid. “Secular” here means that the instability depends on dissipative processes and grows on a long dissipative time scale. In particular, the Dedekind-like bar mode, which has zero eigenfrequency at t = 0.1376 as viewed in the nonrotating frame, is unstable due to gravitational radiation (Chandrasekhar 1970).


Sign in / Sign up

Export Citation Format

Share Document