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Sunday, December 29, 2019

Interesting papers about cosmic rays/turbulence (updating)

// indicates my comments.



book: Physics of space environment
// drift velocity

//https://www.kaggle.com/code/adminpretaktovaniesk/cosmic-rays-spectra-ams-02-daily-fluxes-prl-2021

// poster

Cosmic Ray Feedback on Bi-stable ISM Turbulence
// two zone diffusion coefficient

// apply to study the particle transport

A new model for including galactic winds in simulations of galaxy formation
// apply to interaction of heliosphere and ISM

// note 21, apply to pwn 

// apply to pwn wind, galactic wind, snr wind

// detail of finite difference method

Advanced numerical techniques for time integration of relativistic equations of motion for charged particles
// add turbulence and discuss the suppression of drift

A perturbation approach to a nonlinear advection diffusion equation of particle transport

Cosmic ray interstellar propagation tool using Itoˆ Calculus (CRIPTIC)
// nonlinear cosmic ray propagation

https://github.com/msolanik/Geliosphere
// 2D solar modulation solver

INTRODUCTION TO THE TRANSFER THEORY OF TURBULENCE
// free decay of turbulence?

Is the SNR HESS J1731-347 Colliding with Molecular Clouds?

//Bow-shaped magnetic field surround the snr ?
//What happen if snr in a cloud which has bow-shaped magnetic field? filter for low energy particles?

//interesting; reduced drift velocity
//two new alternative derivations of the equation of transport for cosmic-ray particles in the interplanetary region




Escape of cosmic-ray electrons from supernova remnants 

Supernova shock acceleration of cosmic rays in the Galaxy
// cosmic rays are reaccelerated by other snr again.
Diffusive shock acceleration in modified shocks
//solution to the cosmic ray modified shock accerelation.

 On the plasma temperature in supernova remnants with cosmic-ray modified shocks
//how does it change with wave dissipation. How does it influence the observations.

Time-dependent diffusive acceleration of test particles at shocks 
// apply this method to investigate the cosmic ray propagation time in the galaxy.

Escaping the accelerator: how, when and in what numbers do cosmic raysget out of supernova remnants

Limits on diffusive shock acceleration in dense and incompletely ionised media
// model the particle spectrum inside the molecular cloud.

The microphysics of collisionless shock waves
The Origin of Galactic Cosmic Rays
// to find some ideas

Simplified models for the evolution of supernova remnants including particle acceleration
// is there a parameter could be related to electron/proton ratio (pressure is dominated by proton)?
// can it deduce the e/p ratio ?

NONLINEAR SHOCK ACCELERATION AND PHOTON EMISSION IN SUPERNOVA REMNANTS

https://fenix.tecnico.ulisboa.pt/downloadFile/395144667265/dissertacao.pdf
A good introduction to solar modulation.

STEADY-STATE SOLUTIONS IN NONLINEAR DIFFUSIVE SHOCK ACCELERATION
//particle acceleration and spatial escape.

Spectrum of Electrons Accelerated in Supernova Remnants


CRASH (Cosmic-Ray Amr SHock) code

Transport of magnetic turbulence in supernova remnants



// determined the termination shock position
// this can be used to find the termination shock in the pwn, since the cosmic ray pressure is mainly from proton, we can determine the electron and proton ratio in the pwn. The experiments can give the position of termination shock.
// the time variable hemispherical termination shock
// snr precursor, pwn 
// pre-existing turbulence  

// the compression of magnetic field in SNR

//The  magnetic field distribution and shock property

// good paper for focused transport eqn



// galactic wind cosmic ray accerelation and propagation


//  determine the terminal shock position important for solar modulation.


// get spatial dependent galactic wind speed

// discussed the spatial distribution of the magnetic field in snr

Very interesting

// ! work on this project




// revisit the multiply shock solution.

// fermi bubble ?

// apply to snr


// interesting


// apply this model to expect multiband emission spatial distribution, if compared to observation, have chance to constraint the diffusion coefficient in pwn



// cosmic rays halo around SNR/pwn


// curvature radio emission spectrum due to smooth shock structure
// constraint for nonlinear shock acceleration/ shock structure

// shock structure, turbulence transport, shock acceleration

// how about include new turbulence model and turbulence source



//  isotropic CR spectrum  
// combine with ellen's anisotropy paper



// a proper description of cosmic-ray propagation can only be achieved by using a turbulence-level-dependent diffusion coefficient and can contribute to solving the Galactic cosmic-ray gradient problem

// distance dependended diffusion coefficient
// explain cosmic ray halo in snr/pwn


Cosmic-ray propagation in the bi-stable interstellar medium
// relation between rms(v) and scale R; magnetic field B and density n

// cosmic rays in the molecular cloud

EFFECTS OF NEUTRAL HYDROGEN ON COSMIC-RAY PRECURSORS
IN SUPERNOVA REMNANT SHOCK WAVES
// interesting

// The author think $k_{\perp}/k_{\parallel} \sim 10^{-5}$ is too small and not reasonable.
// They think diffusion coefficient in local interstellar should be smaller.

// galactic wind!

//The evolution of the frozen-in magnetic field in SNR, solve the induction equation

// combine Zweibel's pressure anisotropic instability, see the cosmic rays transport

// derive the turbulence power density equation

// to derive a new transport model for compressible turbulence !!!

// investigate the post-shock structure !!! 



// good introduction

// constraint the local crs sources

// analytic solution for DSA, may extend to spatial dependent diffusion coefficient

// analytic solution for shock structure, spatial dependent averaged diffusion coefficient,  involving the energetic particles escape.
// could be extend to involving the energetic particle viscosity !

Existence and interpretation of smooth cosmic-ray dominated shock structures in supernova remnants
//  turbulence damping formulas

// review, derive diffusion coefficient

https://www.essoar.org/pdfjs/10.1002/essoar.10510106.1
// analytic solution for spatial dependent shock speed and diffusion coefficient, with escape

https://www.aanda.org/articles/aa/full/2003/23/aa3446/aa3446.right.html
// derive the spectrum index for smooth shock structure, could be expand to momentum dependent diffusion coefficient

Pressure anisotropy and small spatial scales induced by velocity shear
https://journals.aps.org/pre/pdf/10.1103/PhysRevE.93.053203?casa_token=wADjnoWjBIAAAAAA%3ACF6bS5OkF8c6NzMWn0i8RzV6Lb6fwLK5vF2z9gpveqZrvxANfQ34R0Swk2zKFq7U2cVp5Tsx2CXM
// extend to cosmic ray distribution function f_2 ?

https://arxiv.org/pdf/2202.07063.pdf
Cosmic-ray propagation and production of secondary particles in the Galaxy (phd thesis)


https://www.issibern.ch/teams/studyshock/Articles/Marcowith06.pdf
// spectrum index of particle for modified shock

// acceleration at oblique shock, new numerical method to solve acceleration eqn.

// analystic modified shock structure and spectrum index

reproducing the Voyager observations required a dramatic change in the diffusion coefficient between the heliosheath and VLISM K_||/K_{\perp} increase by a factor 10^10.Re-creating and understanding the the full implications of the cosmic ray behavior across the heliopause remains a challenge for most models,
// note the change of compressive turbulence to incompressible turbulence (Zank et al. 2019), is this responsible for the change of diffusion coefficient?

Self-confinement of low-energy cosmic rays around supernova remnants
// summary the formulas of turbulence damping.

Charge transfer in proton–helium collisions from low to high energy
// summary of charge exchange cross section, analytic expression

// apply to diffusion shock acceleration on supernova remanants ?

// update ?

// cosmic ray hydrodynamic 

//R. A. Caballero-Lopez,H. Moraal 2004
//H. Moraal 2013

// reproduce the formulas

CAN IBEX IDENTIFY VARIATIONS IN THE GALACTIC ENVIRONMENT OF THE SUN USING ENERGETIC NEUTRAL ATOMS
// sun in the cloud environment ? How this change cosmic ray flux?

// apply to SNR shock or interplanetary shock

//solved Focus transport eq


// used magnetic re-connection acceleration model to explain the observation
// add energy dependent escape time to the magnetic reconnection acceleration model.

// voyager 2 derive the ratio of flow rate and protons loss rate 




https://github.com/piernik-dev
// cosmic ray solver

 
THE DENSITY SPIKE IN COSMIC-RAY MODIFIED SHOCKS: FORMATION, EVOLUTION, AND INSTABILITY
// CR density pike drives the RT instability, and enhance the turbulence ? 

Simulations of cosmic ray propagation
// cosmic ray fluid numerical method review

// discussion about various evolution equation for distribution function
// e.g. Ellen (2019), Zank (2014)
// https://articles.adsabs.harvard.edu/pdf/1987ApJ...315..425K
// Particle acceleration at oblique shock fronts

// Zank 2014
// termination shock, ACR spectra index 

COSMIC-RAY PITCH-ANGLE SCATTERING IN IMBALANCED MHD TURBULENCE SIMULATIONS
// D_{\mu\mu} for the case involving cross helicity
// extend Ellen 2019, Zank 2014

Alternative formulation of weak magnetohydrodynamic turbulence theory
// extend to near incompressible turbulence



// different behaviors for perpendicular and parallel diffusion coefficient at high rigidities. 

Sensitivity of the GAPS experiment to low-energy cosmic-ray antiproton
// low energy antiproton data 105 days

arxiv.org/abs/1412.3773 
Distinguishing Cause From Effect Using Observational Data: Methods And Benchmarks

// old snr 15 pc

An analytical model of turbulence in Parker spiral geometry and associated magnetic field line lengths
// apply to sep transportation

https://markus-x-buchholz.medium.com/brownian-motion-langevin-equation-in-c-8ef79de7ec55
// sde

How Alfvén waves energize the solar wind: heat versus work
// redo it


// sep 

 MAGIX provides a framework to easily interface existing codes to an iterating engine that allows automatic minimizations to constrain model parameters and provide error estimates.


https://astro-staff.uibk.ac.at/~kissmrbu/cronos.html
// solve 3D turbulence transport eq with cronos code
// sep/gcr transportation


// ACE CRIS

// check the Parker and Modified magnetic field model by Ulysses measurements both in solar minimal and solar maximum.

// redo to investigate the role of turbulence pressure

// psp + sod 


// solve mhd eqs

// Frontiers of Physics

// redo with incompressible turbulence spectrum transport eq


// derive the injection threshold for dsa

A global MHD solar wind model with WKB Alfvn waves- Comparison with Ulysses data
// An approximate analytic solution to the coupled problems of coronal heating and solar-wind acceleration
// derive analytic solution of turbulence transport model 


// pwn halo

// an example of lecture note on arxiv

//infer analytical physical laws from data points


Energy Transfers in Fluid Flows: Multiscale and Spectral Perspectives
// a book

2023 APS Career Mentoring Fellow Application
// Mon, Aug 21

pwn evolution and particle

Anisotropic Magnetic Turbulence in the Inner Heliosphere—Radial Evolution of Distributions Observed by Parker Solar Probe
// compared to analytic solution

// correlation function with source

// gcr radial and latitude gradient


https://arxiv.org/abs/2309.00533
// good example of abstract

// good example of ppt

Introduction to plasma physics

https://courses.physics.ucsd.edu/2014/Winter/physics235/Davidson-Loitsyansky%20Problem.pdf
// example for writing a comment

// study cosmic ray diffusion coefficient in the source



// only parallel shock is discussed, extend to oblique shock
at
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