Abstract:I discuss the physics of non-Abelian plasmas which are locally anisotropic in momentum space. Such momentum-space anisotropies are generated by the rapid longitudinal expansion of the matter created in the first 1 fm/c of an ultrarelativistic heavy ion collision. In contrast to locally isotropic plasmas anisotropic plasmas have a spectrum of soft unstable modes which are characterized by exponential growth of transverse chromomagnetic/-electric fields at short times. This instability is the QCD analogue of the… Show more
“…Weibel instabilities are also excited in relativistic plasmas (Yoon and Davidson, 1987) and for relativistic shocks (Milosavljević et al, 2006). This type of instability is even derived from electroweak (Silva et al, 2000) and quark-gluonen plasmas (Arnold and Moore, 2006;Strickland, 2007) and is considered as an alternative source for quasi-stationary magnetic fields besides dynamos (Treumann and Baumjohann, 2012). Furthermore, in gyrotropic or unmagnetized plasmas the existence of a pure growing mode has also been shown based on general linear fluctuation theory and fluctuation-dissipation theorems .…”
Section: Instabilitiesmentioning
confidence: 99%
“…5 (left) and the solar wind velocity as group velocity yielding L char = u 0SW /γ c ≈ 1000-1700 km ≈ L Amp . Hence, the modified ion-Weibel instability is a convective instability (Sturrock, 1958) propagated by the solar wind.…”
Abstract. We analytically discuss wave excitation in a homogeneous three component plasma consisting of solar wind protons, electrons and a beam of cometary water ions applied to the plasma environment of comet 67P/Churyumov-Gerasimenko. The resulting dispersion relations are studied in a solar wind rest frame, where a cometary current is solely generated by the water ion beam, and a cometary rest frame representing the rest frame of the Rosetta spacecraft. A modified ion-Weibel instability is excited by the cometary current and predominantly grows perpendicular to this current. The corresponding water ion mode is connected to a frequency of about 40 mHz in agreement with wave measurements of Rosetta's magnetometer in the cometary rest frame. Furthermore, the superposition of the strongest growing waves result in a fan-like phase structure close to the comet.
“…Weibel instabilities are also excited in relativistic plasmas (Yoon and Davidson, 1987) and for relativistic shocks (Milosavljević et al, 2006). This type of instability is even derived from electroweak (Silva et al, 2000) and quark-gluonen plasmas (Arnold and Moore, 2006;Strickland, 2007) and is considered as an alternative source for quasi-stationary magnetic fields besides dynamos (Treumann and Baumjohann, 2012). Furthermore, in gyrotropic or unmagnetized plasmas the existence of a pure growing mode has also been shown based on general linear fluctuation theory and fluctuation-dissipation theorems .…”
Section: Instabilitiesmentioning
confidence: 99%
“…5 (left) and the solar wind velocity as group velocity yielding L char = u 0SW /γ c ≈ 1000-1700 km ≈ L Amp . Hence, the modified ion-Weibel instability is a convective instability (Sturrock, 1958) propagated by the solar wind.…”
Abstract. We analytically discuss wave excitation in a homogeneous three component plasma consisting of solar wind protons, electrons and a beam of cometary water ions applied to the plasma environment of comet 67P/Churyumov-Gerasimenko. The resulting dispersion relations are studied in a solar wind rest frame, where a cometary current is solely generated by the water ion beam, and a cometary rest frame representing the rest frame of the Rosetta spacecraft. A modified ion-Weibel instability is excited by the cometary current and predominantly grows perpendicular to this current. The corresponding water ion mode is connected to a frequency of about 40 mHz in agreement with wave measurements of Rosetta's magnetometer in the cometary rest frame. Furthermore, the superposition of the strongest growing waves result in a fan-like phase structure close to the comet.
“…In the static limit, for small θ n some of the scales appearing in the dispersion relations are negative implying that the whole system is unstable with respect to magnetic instability [17,18]. It has been demonstrated that in case of k n(θ n = 0), the growth rate of the filamentation instabilities is the largest [10,11,15].…”
We discuss the collective modes due to the propagation of two oppositely moving relativistic jets (dijet) in an anisotropic quark-gluon plasma(AQGP) and compare the results with the case of single jet propagation. For the sake of simplicity, assuming a tsunami-like initial jet distribution, we observe that the dispersion relations for both the stable and unstable modes are altered significantly due to the passage of dijet in comparison with the case of single jet propagation. It has been further demonstrated that the growth rate of instability, due to introduction of dijet in the system, increases compared to the case of single jet case. As in the case of single jet propagation, the instability always grows when the jet velocity is perpendicular to the wave vector. We, thus, argue that the introduction of dijet in the AQGP, in general, leads to faster isotropization than single jet propagation.
“…Strikland presented arguments that during the Glasma phase, the initially approximately boost invariant distribution of particles is unstable with respect to formation of rapidity dependent density fluctuations [20]. The seeds of these fluctuations arise in the quantum wavefunctions for the hadrons, and over time become amplified to a magnitude typical of the Glasma fields.…”
Section: Matter In the Earliest Stages Of Hadronic Collisiosmentioning
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