RDM Stars - Revision history

Emma Platts at 11:19, 27 November 2019

2019-11-27T11:19:18Z

← Older revision		Revision as of 07:19, 27 November 2019
Line 18:		Line 18:
	\|GWCounterpart = ---		\|GWCounterpart = ---
	\|NeutrinoCounterpart = ---		\|NeutrinoCounterpart = ---
	\|References = https://arxiv.org/pdf/1812.11801.~~pdf~~		\|References = https://arxiv.org/pdf/1812.11801, https://arxiv.org/abs/1906.09074
	\|Comments = Repeaters are possible if multiple asteroids collide with the star		\|Comments = Repeaters are possible if multiple asteroids collide with the star
	}}		}}
Line 28:		Line 28:
	== Observational Constraints ==		== Observational Constraints ==

	~~The RDM stars considered in this model are assumed to be located in the centers of galaxies~~.		None.

Emma Platts: /* Model Description */

2019-09-05T18:00:13Z

Model Description

← Older revision		Revision as of 14:00, 5 September 2019
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	This model considers a radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.		This model considers radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.

	== Observational Constraints ==		== Observational Constraints ==

	The RDM stars considered in this model are assumed to be located in the centers of galaxies.		The RDM stars considered in this model are assumed to be located in the centers of galaxies.

Emma Platts: Created page with " {{FRBTableTemplate |Category = Other |Pro..."

2019-09-05T11:36:40Z

Created page with "   {{FRBTableTemplate |Category = Other |Pro..."

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = RDM Star
|Type = Both
|EnergyMechanism = Stimulated emission
|EmissionMechanism = Synch.
|LFRadioCounterpart = ---
|HFRadioCounterpart = ---
|MicrowaveCounterpart = ---
|THzCounterpart = ---
|OIRCounterpart = ---
|XrayCounterpart = ---
|GammarayCounterpart = ---
|GWCounterpart = ---
|NeutrinoCounterpart = ---
|References = https://arxiv.org/pdf/1812.11801.pdf
|Comments = Repeaters are possible if multiple asteroids collide with the star
}}

== Model Description ==

This model considers a radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.

== Observational Constraints ==

The RDM stars considered in this model are assumed to be located in the centers of galaxies.