Merge branch 'main' of github.com:PlasmaPy/PlasmaPy-Demos

Author: namurphy

2023-SULI/README.md

@@ -12,7 +12,8 @@ Notebooks for this workshop can be run in three ways:
 
 3. On a **local installation of Python** that includes Jupyter notebook. (Advanced)
 
-Note that some functionality, like interactive plots, may not work on Google Colaboratory. Instructions are included below for each option.
+Some functionality, like interactive plots, may not work on Google Colaboratory. Instructions are included below for each option.
+
 
 # Table of contents
 
@@ -47,6 +48,11 @@ Once the Binder enviroment has initialized, navigate to the folder with the name
 # Running Examples on Jupyter Notebook Locally with Anaconda <a name="installation_anaconda"></a>
 1. Download the .ipynb file for the notebook(s)
 
+   The notebooks can be downloaded from Google Drive at the following links. Click on the link and select "Download".
+
+   - [Getting started with PlasmaPy](https://drive.google.com/file/d/1xf4M64Xp6e2tfo17W2Pm_6B1jzPy4L36/view?usp=sharing)
+   - [Single particle drifts](https://drive.google.com/file/d/1tAXZOF3_TD5CBMsE_6eDdP_-M95_vcRD/view?usp=sharing)
+
 2. Download and install [Anaconda](https://www.anaconda.com/download)
 
 3. Open Anaconda and do the following to create a new enviroment with PlasmaPy and all its dependencies installed.
@@ -55,7 +61,7 @@ Once the Binder enviroment has initialized, navigate to the folder with the name
 
   b) Left click on the green arrow.
 
-  c) Click'Open Terminal' to open a command prompt.
+  c) Click 'Open Terminal' to open a command prompt.
 
 ![anaconda_open_terminal](https://github.com/PlasmaPy/PlasmaPy-Demos/assets/32618747/a3054200-13ff-4d85-937e-0b379976536f)
 
@@ -73,11 +79,10 @@ Once the Binder enviroment has initialized, navigate to the folder with the name
 
 ![anaconda_open_enviroment](https://github.com/PlasmaPy/PlasmaPy-Demos/assets/32618747/cb23fa79-3f35-4f4b-8df1-7b6cb16d3af2)
 
-6. Click 'Launch' on the Jupyter Notebook card. The program should open in your default web browser. Navigate to the downloaded .ipynb file and click on the title to open the notebook. ![anaconda_open_notebook](https://github.com/PlasmaPy/PlasmaPy-Demos/assets/32618747/67fa8cf0-4d92-4dc9-bee0-175dcd1d7f0f)
-
-  
+6. Click 'Launch' on the Jupyter Notebook card. The program should open in your default web browser. Navigate to the downloaded `.ipynb` file and click on the title to open the notebook. ![anaconda_open_notebook](https://github.com/PlasmaPy/PlasmaPy-Demos/assets/32618747/67fa8cf0-4d92-4dc9-bee0-175dcd1d7f0f) 
 
 # Tips on Using Jupyter Notebook <a name="jupyter_tips"></a>
+
 - Select "Runtime>Run All" to run the entire notebook. 
 - To run a single cell, select the cell with your mouse and then press "Shift+Enter"
 - Create new cells using the "Insert" menu or the "+Code" button.

2023-SULI/plasmapy-tutorial-completed.ipynb

@@ -5,7 +5,7 @@
    "id": "5b8f9968",
    "metadata": {},
    "source": [
-    "# PlasmaPy"
+    "# SULI Computational Workshop"
    ]
   },
   {
@@ -30,6 +30,12 @@
    "metadata": {},
    "outputs": [],
    "source": [
+    "import sys\n",
+    "\n",
+    "if 'google.colab' in str(get_ipython()):\n",
+    "    if 'plasmapy' not in sys.modules:\n",
+    "        !pip install plasmapy==2023.5.1 requests==2.27.1\n",
+    "        \n",
     "import numpy as np\n",
     "import astropy.units as u\n",
     "from astropy import constants as const\n",
@@ -931,7 +937,11 @@
    "metadata": {},
    "outputs": [],
    "source": [
-    "electron.is_category(require=\"lepton\", exclude=\"baryon\", any_of={\"boson\", \"fermion\"})"
+    "electron.is_category(\n",
+    "    require=\"lepton\", \n",
+    "    exclude=\"baryon\", \n",
+    "    any_of={\"boson\", \"fermion\"},\n",
+    ")"
    ]
   },
   {
@@ -1129,7 +1139,7 @@
    "id": "0ba578e6",
    "metadata": {},
    "source": [
-    "When we calculate $β$ for the photosphere, we find that it is an order of magnitude larger than 1, so plasma pressure forces are more important than magnetic tension and pressure."
+    "When we calculate $β$ for the photosphere, we find that it is an order of magnitude larger than $1$, so plasma pressure forces are more important than magnetic tension and pressure."
    ]
   },
   {
@@ -1178,7 +1188,7 @@
     "\n",
     "[Magnetic reconnection] is the fundamental plasma process that converts stored magnetic energy into kinetic energy, thermal energy, and particle acceleration.  Reconnection powers solar flares and is a key component of geomagnetic storms in Earth's magnetosphere. Reconnection can also degrade confinement in fusion devices such as tokamaks.\n",
     "\n",
-    "The **inertial length** for a particle is the characteristic length scale for getting accelerated or decelerated by forces in a plasma.  \n",
+    "The **inertial length** is the characteristic length scale for a particle to get accelerated or decelerated by electromagnetic forces in a plasma.  \n",
     "\n",
     "When the reconnection layer thickness is shorter than the **ion inertial length**, $d_i ≡ c/ω_{pi}$, collisionless effects and the Hall effect enable reconnection to be **fast** (Zweibel & Yamada 2009).  The inner electron diffusion region has a thickness of about the **electron inertial length**, $d_e≡c/ω_{pe}$.  (Here, $ω_{pi}$ and $ω_{pe}$ are the ion and electron plasma frequencies.)\n",
     "\n",
@@ -1367,7 +1377,7 @@
    "name": "python",
    "nbconvert_exporter": "python",
    "pygments_lexer": "ipython3",
-   "version": "3.10.10"
+   "version": "3.11.3"
   },
   "widgets": {
    "application/vnd.jupyter.widget-state+json": {

2023-SULI/plasmapy-tutorial.ipynb

@@ -1079,7 +1079,7 @@
     "\n",
     "[Magnetic reconnection] is the fundamental plasma process that converts stored magnetic energy into kinetic energy, thermal energy, and particle acceleration.  Reconnection powers solar flares and is a key component of geomagnetic storms in Earth's magnetosphere. Reconnection can also degrade confinement in fusion devices such as tokamaks.\n",
     "\n",
-    "The **inertial length** for a particle is the characteristic length scale for getting accelerated or decelerated by forces in a plasma.  \n",
+    "The **inertial length** is the characteristic length scale for a particle to get accelerated or decelerated by electromagnetic forces in a plasma.  \n",
     "\n",
     "When the reconnection layer thickness is shorter than the **ion inertial length**, $d_i ≡ c/ω_{pi}$, collisionless effects and the Hall effect enable reconnection to be **fast** (Zweibel & Yamada 2009).  The inner electron diffusion region has a thickness of about the **electron inertial length**, $d_e≡c/ω_{pe}$.  (Here, $ω_{pi}$ and $ω_{pe}$ are the ion and electron plasma frequencies.)\n",
     "\n",