Abstract
We use a direct numerical integration of the Vlasov equation in spherical symmetry with a background gravitational potential to determine the evolution of a collection of particles in different models of a galactic halo in order to test its stability against perturbations. Such collection is assumed to represent a dark matter inhomogeneity which is represented by a distribution function defined in phase-space. Non-trivial stationary states are obtained and determined by the virialization of the system. We describe some features of these stationary states by means of the properties of the final distribution function and final density profile. We compare our results using the different halo models and find that the NFW halo model is the most stable of them, in the sense that an inhomogeneity in this halo model requires a shorter time to virialize.
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Notes
When instead of particles moving in an external potential we consider the case of self-gravitating particles, then the virial theorem can also be derived, and in that case we do find that Eq. (2.30) is satisfied with \(n=-1\) since the mutual forces between the particles are purely gravitational.
References
MarrodÃąn Undagoitia, T., Rauch, L.: Dark matter direct-detection experiments. J. Phys. G43(1), 013001 (2016). doi:10.1088/0954-3899/43/1/013001
Akerib, D.S., et al.: The large underground xenon (LUX) experiment. Nucl. Instrum. Methods A704, 111 (2013). doi:10.1016/j.nima.2012.11.135
Bernabei, R., et al.: The DAMA/LIBRA apparatus. Nucl. Instrum. Methods A592, 297 (2008). doi:10.1016/j.nima.2008.04.082
Akimov, D.Y., et al.: The ZEPLIN-III dark matter detector: instrument design, manufacture and commissioning. Astropart. Phys. 27, 46 (2007). doi:10.1016/j.astropartphys.2006.09.005
Aprile, E., Angle, J., Arneodo, F., Baudis, L., Bernstein, A., Bolozdynya, A., Brusov, P., Coelho, L.C.C., Dahl, C.E., DeViveiros, L., Ferella, A.D., Fernandes, L.M.P., Fiorucci, S., Gaitskell, R.J., Giboni, K.L., Gomez, R., Hasty, R., Kastens, L., Kwong, J., Lopes, J.A.M., Madden, N., Manalaysay, A., Manzur, A., McKinsey, D.N., Monzani, M.E., Ni, K., Oberlack, U., Orboeck, J., Orlandi, D., Plante, G., Santorelli, R., dos Santos, J.M.F., Shagin, P., Shutt, T., Sorensen, P., Schulte, S., Tatananni, E., Winant, C., Yamashita, M.: Design and performance of the XENON10 dark matter experiment. Astropart. Phys. 34, 679 (2011). doi:10.1016/j.astropartphys.2011.01.006
Barreto, J., et al.: Direct search for low mass dark matter particles with CCDs. Phys. Lett. B 711, 264 (2012). doi:10.1016/j.physletb.2012.04.006
Chavarria, A.E., et al.: DAMIC at SNOLAB. Phys. Procedia 61, 21 (2015). doi:10.1016/j.phpro.2014.12.006
Aguilar-Arevalo, A., et al.: First direct detection constraints on eV-scale hidden-photon dark matter with DAMIC at SNOLAB. Phys. Rev. Lett. (2016) (submitted to)
Aguilar-Arevalo, A., et al.: Search for low-mass WIMPs in a 0.6 kg day exposure of the DAMIC experiment at SNOLAB. Phys. Rev. D 94(8), 082006 (2016). doi:10.1103/PhysRevD.94.082006
Agnese, R., et al.: Low-Mass Dark Matter Search with CDMSlite. Phys. Rev. D (2017) (submitted to)
de Lima Rodrigues, R.: The quantum mechanics SUSY algebra: an introductory review (2002)
Cabral-Rosetti, L.G., Mondragon, M., Reyes Perez, E.: Toroidal dipole moment of the lightest neutralino in the MSSM. J. Phys. Conf. Ser. 315, 012007 (2011). doi:10.1088/1742-6596/315/1/012007
Biswas, S., Gabrielli, E., Heikinheimo, M., Mele, B.: Dark-photon searches via Higgs-boson production at the LHC. Phys. Rev. D 93(9), 093011 (2016). doi:10.1103/PhysRevD.93.093011
Barranco, J., Bernal, A., Núñez, D.: Dark matter equation of state from rotational curves of galaxies. Mon. Not. R. Astron. Soc. 449(1), 403 (2015). doi:10.1093/mnras/stv302
Matos, T., Guzman, F.S., Urena-Lopez, L.A.: Scalar field as dark matter in the universe. Class. Quantum Gravity 17, 1707 (2000). doi:10.1088/0264-9381/17/7/309
Matos, T., Urena-Lopez, L.A.: Scalar field dark matter, cross section and Planck-scale physics. Phys. Lett. B 538, 246 (2002). doi:10.1016/S0370-2693(02)02002-6
Matos, T., Bernal, A., Nunez, D.: Flat central density profiles from scalar field dark matter halo. Rev. Mex. Astron. Astrofis. 44, 149 (2008)
Navarro, J.F., Frenk, C.S., White, S.D.M.: The structure of cold dark matter halos. Astrophys. J. 462, 563 (1996). doi:10.1086/177173
Harker, G., Cole, S., Helly, J., Frenk, C., Jenkins, A.: A marked correlation function analysis of halo formation times in the millennium simulation. Mon. Not. R. Astron. Soc. 367, 1039 (2006). doi:10.1111/j.1365-2966.2006.10022.x
Athanassoula, E., Fady, E., Lambert, J.C., Bosma, A.: Optimal softening for force calculations in collisionless N-body simulations. Mon. Not. R. Astron. Soc. 314(3), 475 (2000). doi:10.1046/j.1365-8711.2000.03316.x
Dehnen, W.: Towards optimal softening in three-dimensional N-body codes I. Minimizing the force error. Mon. Not. R. Astron. Soc. 324(2), 273 (2001). doi:10.1046/j.1365-8711.2001.04237.x
Hockney, R.W., Eastwood, J.W.: Computer simulation using particles. Hilger, Bristol (1988). http://adsabs.harvard.edu/abs/1988csup.book.....H
Bagla, J.S.: Cosmological N-body simulation: techniques, scope and status. Curr. Sci. 88, 1088 (2005)
Binney, J., Tremaine, S.: Galactic dynamics, 2nd edn. Princeton University Press, Princeton, NJ, USA (2008). http://adsabs.harvard.edu/abs/2008gady.book.....B
Colombi, S., Sousbie, T., Peirani, S., Plum, G., Suto, Y.: Vlasov versus N-body: the Henon sphere. Mon. Not. R. Astron. Soc. 450(4), 3724 (2015). doi:10.1093/mnras/stv819
Andreasson, H.: The Einstein–Vlasov system/kinetic theory. Living Rev. Rel. 8, 2 (2005). doi:10.12942/lrr-2005-2
Shapiro, S.L., Teukolsky, S.A.: Black holes, white dwarfs, and neutron stars: the physics of compact objects. Research supported by the National Science Foundation, Wiley, New York (1983). http://adsabs.harvard.edu/abs/1983bhwd.book.....S
Domínguez-Fernández, P.: On particle dynamics: Vlasov equation and dark matter. Bachelor thesis, UNAM-Mexico (2015)
Jiménez-Vázquez, E.: Numerical simulation of the Vlasov–Poisson system in spherical symmetry. Bachelor thesis, UNAM-Mexico (2016)
Kuzio de Naray, R., McGaugh, S.S., Mihos, J.C.: Constraining the NFW potential with observations and modeling of LSB galaxy velocity fields. Astrophys. J. 692, 1321 (2009). doi:10.1088/0004-637X/692/2/1321
Salucci, P., Burkert, A.: Dark matter scaling relations. Astrophys. J. 537, L9 (2000). doi:10.1086/312747
Liu, W.H., Fu, Y.N., Deng, Z.G., Huang, J.H.: An equilibrium dark matter halo with the Burkert profile. Publ. Astron. Soc. Jpn. 57, 541 (2005). doi:10.1093/pasj/57.4.541
Rubin, V.C., Thonnard, N., Ford Jr., W.K.: Rotational properties of 21 SC galaxies with a large range of luminosities and radii, from NGC 4605 /R = 4kpc/ to UGC 2885 /R = 122 kpc/. Astrophys. J. 238, 471 (1980). doi:10.1086/158003
Leveque, R.J.: Numerical Methods for Conservation Laws. Birkhauser Verlag, Basel (1992)
Barranco, J., Bernal, A., Degollado, J.C., Diez-Tejedor, A., Megevand, M., et al.: Are black holes a serious threat to scalar field dark matter models? Phys. Rev. D 84, 083008 (2011). doi:10.1103/PhysRevD.84.083008
Barranco, J., Bernal, A., Degollado, J.C., Diez-Tejedor, A., Megevand, M., et al.: Schwarzschild black holes can wear scalar wigs. Phys. Rev. Lett. 109, 081102 (2012). doi:10.1103/PhysRevLett.109.081102
Barranco, J., Bernal, A., Degollado, J.C., Diez-Tejedor, A., Megevand, M., et al.: Schwarzschild scalar wigs: spectral analysis and late time behavior. Phys. Rev. D 89(8), 083006 (2014). doi:10.1103/PhysRevD.89.083006
Martin-Garcia, J.M., Gundlach, C.: Selfsimilar spherically symmetric solutions of the massless Einstein–Vlasov system. Phys. Rev. D 65, 084026 (2002). doi:10.1103/PhysRevD.65.084026
Akbarian, A., Choptuik, M.W.: Critical collapse in the spherically-symmetric Einstein–Vlasov model. Phys. Rev. D 90(10), 104023 (2014). doi:10.1103/PhysRevD.90.104023
Acknowledgements
This work was partially supported by DGAPA-UNAM Grant IN103514, by CONACYT Network Project 280908 “Agujeros Negros y Ondas Gravitatorias”, and by Conacyt Grant Fronteras 281.
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Kinetic theory
Kinetic theory
1.1 Zero angular momentum
When the motion is purely radial and the angular momentum is zero, \(L_0=0\), the derivation of the particle density \(\rho _f\) in physical space, the momentum density \(j_f\), the mean value over momentum space, the average value of an arbitrary function g, and the total number of particles has to begin with a Dirac delta dependence of the distribution function in the angular momenta
Transforming the Dirac deltas from coordinates (\(p_\theta \),\(p_\varphi \)) to the new coordinates (L,\(\psi \)) yields
So that the expressions for the density, current, mean value and average in the case of zero angular momentum become
1.2 Continuity equation
We start from the Vlasov equation written as
where \(\varPhi _{\mathrm{eff}}(r) \equiv \varPhi (r)+ L^2/2 m r^2\) is the effective potential. Integrating over momentum space we find
with \(d \bar{\omega }\) the volume element given in Eq. (2.7).
For now on we will assume that the distribution function is of compact support in phase space (or decays very rapidly). The first term of the above equation is easy to simplify:
where have used the definition of the particle density \(\rho _f\), Eq. (2.9). In a similar way we find for the second term:
where we have now used the definition of the momentum density \(j_f\), Eq. (2.10). Finally, the last term can be easily shown to vanish for a distribution function of compact support:
where we assumed that f is zero for large values of \(|p_r|\). If we now define the mass density as \(\rho _m := m \rho _f\), the Vlasov equation integrated over momentum space reduces to
which is nothing more than the standard continuity equation in spherical symmetry. By integrating the continuity equation in physical space it can now be easily shown, by using the divergence theorem, that the number of particles N defined above in Eq. (2.12) is conserved in the sense that \(\partial N / \partial t = 0\).
1.3 Virial theorem
To obtain the virial theorem, the Vlasov equation in spherical symmetry is multiplied by \(r p_r\), and integrated over phase space:
The first term above can be rewritten as:
For the second term in Eq. (A.14) we find:
where in the second line above we integrated by parts over r, using the fact that f has compact support, and where \(K_r=p_r^2/2m\) is the radial kinetic energy.
For the third term of (A.14) we find:
where again we have integrated by parts, but now over \(p_r\), and where we defined the effective force as \(F_{\mathrm{eff}}(r) = - \partial \varPhi _{{\mathrm{eff}}}(r) / \partial r\).
Collecting our results we find that the integrated Vlasov equation becomes
The last result is known as the virial theorem. In a steady state, the virial theorem implies
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Domínguez-Fernández, P., Jiménez-Vázquez, E., Alcubierre, M. et al. Description of the evolution of inhomogeneities on a dark matter halo with the Vlasov equation. Gen Relativ Gravit 49, 123 (2017). https://doi.org/10.1007/s10714-017-2286-8
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DOI: https://doi.org/10.1007/s10714-017-2286-8