.. _sphx_glr_api_gallery_relativity_neutron_star:

Neutron stars
--------------

The Tolman-Oppenheimer-Volkoff equations and the maximum neutron star mass.


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  <div id='sg-tag-list' class='sphx-glr-tag-list'></div>


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    <div class="sphx-glr-thumbnails">

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    <div class="sphx-glr-thumbcontainer" tooltip="Oppenheimer and Volkoff&#x27;s 1939 relativistic generalization of hydrostatic equilibrium predicts something Newtonian gravity cannot: a maximum possible mass for a neutron star. The star&#x27;s matter is modeled as a polytrope, P = K\rho_0^\Gamma, relating pressure to rest-mass density, with total energy density (rest mass plus internal energy) \varepsilon = \rho_0 + P/(\Gamma-1). Enclosed mass m(r) and pressure P(r) then obey the Tolman-Oppenheimer-Volkoff equations">

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  .. image:: /api/gallery/relativity/neutron_star/images/thumb/sphx_glr_plot_tov_mass_radius_thumb.png
    :alt:

  :doc:`/api/gallery/relativity/neutron_star/plot_tov_mass_radius`

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      <div class="sphx-glr-thumbnail-title">The neutron star maximum mass: solving the TOV equations</div>
    </div>


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    </div>


.. toctree::
   :hidden:

   /api/gallery/relativity/neutron_star/plot_tov_mass_radius