Transfer [MHz, Jy] to [eV, erg]

#transfer [frequency(MHz), Jy] to [eV, erg/cm^2/s]
import numpy as np import sys                                                                                                                                                             src=sys.argv[1]
mu,F_mu,eF = np.loadtxt(src,usecols=(0,1,2),unpack=True)
with open(src[:src.find('_')]+'_radio.txt','w') as rf:
freq_to_ev = 4.135667516*1e-15 # 1HZ to eV
Jy_to = 1e-23 # Jy to erg/cm^2/s/Hz
for x,y,z in zip(mu,F_mu,eF): 
# for MHz *1e6 to Hz
rf.write(str(x*freq_to_ev*1e6)+'\t'+str(y*x*1e6*Jy_to)+'\t'+str(z*x*1e6*Jy_to)+'\n')

Literates list

1. deduce the magnetic field from filament
MAGNETIC FIELD AMPLIFICATION IN THE THIN X-RAY RIMS OF SN 1006
https://iopscience.iop.org/article/10.1088/0004-637X/790/2/85/meta

2. CRs and cloud
kinetic model for shock particle acceleration in the presence of neutrals
A self-consistent description of shock particle acceleration in the presence of neutral hydrogen
T: Interplay between physics and geometry in Balmer filaments: the case of SN 1006

3.TEMPORAL EVOLUTION OF NON-THERMAL SPECTRA FROM SUPERNOVA REMNANTS
Assuming that supernova shocks accelerate non-thermal particles, we model the temporally evolving non-thermal particle and photon spectra at different stages in the lifetime of a standard shell-type supernova remnant (SNR).
https://iopscience.iop.org/article/10.1086/304894/pdf


4. The efficiency of the pulsar spin-down energy transfer into cosmic rays energy
0.01%–10% range of observed VHE efficiencies for other PWNe (Gallant 2007)
Gallant, Y. A. 2007, Ap&SS, 309, 197G

5.the magnetic field at the shock front is high but rapidly decays toward the inside (Pohl et al. 2005), increasing the synchrotron loss times and increasing the diffusion constant. However, the decay in magnetic field should be reflected in the radio emissivity from the forward shock to the inside,

6.evidence cosmic ray convection in galaxy NCG253
T:cosmic rays and magnetic field in the nearby starburst galaxy ngc 253


7.The interpretation of the narrow filaments as the cooling width of the multi-TeV x-ray emitting electrons implies that similar filaments are not expected in the radio observations.
T:In which shell-type SNRs should we look for gamma-rays and neutrinos from P–P collisions

8.A DECLINE IN THE NONTHERMAL X-RAY EMISSION FROM CASSIOPEIA A
https://iopscience.iop.org/article/10.1088/2041-8205/729/2/L28/pdf
see discussion discuss the variation of radio emission spectra index

9. List of snr interacting with cloud
A SYSTEMATIC SURVEY FOR BROADENED CO EMISSION TOWARD GALACTIC SUPERNOVA REMNANTS

https://iopscience.iop.org/article/10.3847/0004-637X/816/1/1/pdf

tycho no

cas a  yes

ic443 yes


10 detail of solar modulation
https://link.springer.com/content/pdf/10.1023%2FA%3A1010376901322.pdf


11. two solar minimum, ACE energy spectrum
https://openscholarship.wustl.edu/cgi/viewcontent.cgi?article=1706&context=etd


12. Near sun transport equation
In the inner heliosphere, i.e. within about 1 AU, particle propagation is influenced mainly by pitch-angle scattering and focusing. The resulting transport equation then is the focused transport equation
Space physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres

Supernova and Cosmic rays Notes

https://www.aanda.org/articles/aa/pdf/2018/10/aa32879-18.pdf

The magnetic field turbulence created upstream and at the shock by various instabilities is transferred downstream where it is eventually damped due to the lack of the turbulence driving (Pohl et al. 2005).

The immediate downstream magnetic field is transported inside the SNR with the plasma flow and evolves following the induction equation for ideal MHD.

The remnant expanded in a medium with small dense clouds that survive the passage of the shock
and provide target material for cosmic rays. However, this scenario also has diverticulitis large amount of mass in clouds required for a fit of the high energy spectrum in this scenario requires pre-exiting clouds unaffected by the stellar wind of the progenitor star, which is rather implausible as the stellar wind would form kevin-helmholtz and rayleigh-taylor instabilities destroying the outer layers of the clouds. This would be followed by the formation of steams of gas, which would stongle emit x-rays when interacting with the forward shock.

Cosmic ray production in supernovae
https://arxiv.org/pdf/1801.08890.pdf

4.5 Effect of CR acceleration on remnant dynamics, plasma heating, and thermal X-ray production

If CRs are produced efficiently (i.e., > 10% of the shock bulk flow kinetic energy is placed in relativistic particles), the backpressure of CRs will influence the remnant hydrodynamics since relativistic particles produce less pressure for a given energy density than non-relativistic ones.
The energy placed in CRs comes from the thermal plasma so the shocked temperature is less than expected for test-particle acceleration.
Furthermore, the efficient production of CRs can result in an increase in the shock compression ratio from standard Rankine-Hugoniot values.
The change in temperature and density of the shocked plasma will modify the X-ray line emission. This effect has been studied extensively with a code coupling the remnant hydrodynamics with efficient CR production (see Ellison et al. 2012, Patnaude et al. 2017, and references therein). The effect of CR production influences the non-equilibrium ionization X-ray emission in observable ways.


4.6 Magnetic field amplification (MFA)
? the correlation between magnetic field amplifiation and cosmic rays pressure 
? MFA need high cosmic rays pressure (proton is important)
Bykov et al. (2014) giving the pressure in magnetic turbulence versus shock speed u0, as obtained with Monte Carlo techniques including the resonant CR-streaming instability and two non-resonant CR-current instabilities (i.e., Bell 2005, Bykov et al. 2013). The Monte Carlo results show that the efficiency of MFA, as defined by the pressure in turbulence, saturates at ∼ 10 − 15% of the far upstream bulk flow ram pressure.
https://arxiv.org/pdf/1105.0130.pdf (Magnetic fields in cosmic particle acceleration sources)

Wrap text into a shade box in blogger

blockquote {
color: #888;
border: 2px solid #333;
padding: 10px;
background-color: #ccc;
}

put above codes into the style.css.

Or  write below codes in the the html post.

<blockquote style="border: 2px solid #666; padding: 10px; background-color: #ccc;"> This is some quoted text.</blockquote>

Reference:
https://www.bloggingbasics101.com/how-do-i-make-s/
https://www.rapidtables.com/web/color/html-color-codes.html

Tricks on ploting figure with matplotlib

plot error-bar and upper limit

# lower & upper limits of the error
lolims = np.array([0, 0, 1, 0, 1, 0, 0, 0, 1, 0], dtype=bool)
uplims = np.array([0, 1, 0, 0, 0, 1, 0, 0, 0, 1], dtype=bool)

ax.errorbar(x, y + 2.1, xerr=xerr, yerr=yerr,
            xlolims=xlolims, xuplims=xuplims,
            uplims=uplims, lolims=lolims,
            marker='o', markersize=8,
            linestyle='none')

plt.legend(frameon=False)




set ticker in log scale
https://stackoverflow.com/questions/44078409/matplotlib-semi-log-plot-minor-tick-marks-are-gone-when-range-is-large

Reference:
https://matplotlib.org/3.1.0/gallery/statistics/errorbar_limits.html

Build scientific environment with Termux in Chromebook

bashrc
/data/data/com.termux/files/usr/etc/bash.bashrc

open new session
ctrl alt c

to next session
ctrl alt n

download file from google drive
curl gdrive.sh | sh -s https://drive.google.com/open?id=YOUR_SHARE_ID

Google Drive client for the commandline
https://github.com/odeke-em/drive

SSH login without password

a@A:~> ssh-keygen -t rsa

a@A:~> ssh b@B mkdir -p .ssh

a@A:~> cat .ssh/id_rsa.pub | ssh b@B 'cat >> .ssh/authorized_keys'

http://www.linuxproblem.org/art_9.html

add user

sudo adduser mpiu --uid 999

Setting up SSH host shortnames

https://www.howtogeek.com/75007/stupid-geek-tricks-use-your-ssh-config-file-to-create-aliases-for-hosts/


/data/data/com.termux/files/usr/etc/bash.bashrc
show color for different extension
LS_COLORS=$LS_COLORS:'di=1;34:*.c=01;32:*.tex=01,31:*.py=01;35:*.c=01;32:*.pdf=0;36:'
export LS_COLORS

change font color in vim
edit in .vimrc
colo desert
syntax on

Install latex in termux

1) pdflatex: can not found pdflatex.fmt
    texconfig rehash
2) not found  xx.sty
    tlmgr search --global --file xx.sty
    tlmgr install package_name
3) metric file not found
    tlmgr install collection-fontsrecommended


Reference:
https://tex.stackexchange.com/questions/75166/error-in-tex-live-font-not-loadable-metric-tfm-file-not-found