Tariq Rathbone

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This is a beta release. It may contain bugs and problems.

Please be patient while using it and report back any problem you have encountered to https://github.com/orcun-gokbulut/qml-debug/issuess

Thank you for using Qml-Debug Beta.

Short Description: QML Debuger for VSCode.

Detailed Description: Debug Adapter Protocol (DAP), which is used by Visual Studio Code to interface with various debuggers, implementation for Qt QML debugger.

https://microsoft.github.io/debug-adapter-protocol/

Right now only attach mode debugging is supported which means you have to launch your application (by hand or through another Visual Studio Code launch configuration) and then attach Qml Debugger.

This limitation will be lifted in future releases. Qml Debug will eventually gain the ability to launch your application.

Attach mode attaches Qml Debugger in the already running application instance.

Sample launch.json Configuration:

Configuration Properties

In order to Qml Debuger find your source code, you should have one or more path matching options in your configuration. These mapping tuples are contained in configuration's path property.

Example:

In order to debug your Qml based application in attach mode you have to start your binary with debug parameters;

These parameters will instruct Qt to load necessary debugger plugins and extensions. On launch mode Qml Debugger extension will add these paramters automaticly but in attach mode you have to add it yourself when you are launching your application by hand.

You can also use VSCode launch.json configuration to append the parameters by adding flowing lines to your configration;;

If you want use multiple debugger (C++ and Qml) at the same time you should crate compatable one Qml Debug configuıration and one cppdbg configuration then combine them into launch compound.

You should make sure that cppdbg launch configration launches application with debugging command line arguments with correct hostname and port values that matches with your Qml Debug launch configuration.

Command Line Arguments:

-qmljsdebugger=host:localhost,port:12150,services:DebugMessages,QmlDebugger,V8Debugger

Launch Configuration:

"host": "localhost", "port": 12150,

Example compund launch configration;

Project is still in development. Current version is fully functional but unstable with lots of potential bugs. In addition to that, there are rooms for improvements in various places. Therefore, still work in progress...

👤 Y. Orçun Gökbulut

Contributions, issues and feature requests are welcome!Feel free to check issues page. You can also take a look at the contributing guide.

The sun gives energy to life on Earth, and without this star, we wouldn't be here. But even stars have limited lifetimes, and someday our sun will die.

You don't need to worry about this solar death anytime soon, though. Like all stars, a churning fusion engine fuels the sun, and it still has a lot of fuel left — about 5 billion years' worth.

Related: What's inside the sun? A star tour from the inside out

Stars like our sun form when a huge cloud of gas (mostly hydrogen and helium) grows so large that it collapses under its own weight. The pressure is so high in the center of that collapsing mass of gas that the heat reaches unimaginable levels, with temperatures so hot that hydrogen atoms lose their electrons.

Those naked hydrogen atoms then fuse together into helium atoms, and that reaction releases enough energy to counter the intense pressure of gravity collapsing the cloud of gas. The battle between gravity and the energy from fusion reactions fuels our sun and billions of other stars in our galaxy and beyond.

But in about 5 billion years, the sun will run out of hydrogen. Our star is currently in the most stable phase of its life cycle and has been since the formation of our solar system, about 4.5 billion years ago. Once all the hydrogen gets used up, the sun will grow out of this stable phase.

With no hydrogen left to fuse in the core, a shell of fusion hydrogen will form around the helium-filled core, astrophysicist Jillian Scudder wrote in an article for The Conversation. Gravitational forces will take over, compressing the core and allowing the rest of the sun to expand.

Our star will grow to be larger than we can imagine — so large that it will envelope the inner planets, including Earth. That's when the sun will become a red giant, which it will remain for about a billion years.

Then, the hydrogen in that outer core will deplete, leaving an abundance of helium. That element will then fuse into heavier elements, like oxygen and carbon, in reactions that don't emit as much energy. Once all the helium disappears, the forces of gravity will take over, and the sun will shrink into a white dwarf. All the outer material will dissipate, leaving behind a planetary nebula.

"When a star dies, it ejects a mass of gas and dust — known as its envelope — into space. The envelope can be as much as half the star's mass," astronomer Albert Zijlstra of the University of Manchester in the United Kingdom, said in a statement. "This reveals the star's core, which by this point in the star's life is running out of fuel, eventually turning off and before finally dying."

Astronomers estimate that the sun has about 7 billion to 8 billion years left before it sputters out and dies. One way or another, humanity may well be long gone by then.

Our sun isn't massive enough to trigger a stellar explosion, called a supernova, when it dies, and it will never become a black hole either.

In order to create a supernova, a star needs about 10 times the mass of our sun. An object of that size would form a dense stellar corpse called a neutron star after the explosion.

To leave behind a black hole, a supernova must occur in a star with about 20 times the mass of the sun.

Find out what will happen to the Earth when the sun dies, from Live Science. Learn more about how stars form, evolve and die from NASA, and learn more about how the agency studies our sun. Watch a mini documentary on the topic, The Death of the Sun, from PBS Space Time.

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