@daenerya secret gift exchange ❤ for @sardoniyx
» Destiny is something that we’ve invented because we can’t stand that fact that everything that happens is accidental.
↳ Sleepless in Seattle (1993) dir. Nora Ephron

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Cosmic Funnies
Not today Justin
todays bird
RMH
ojovivo

Love Begins
wallacepolsom
YOU ARE THE REASON

titsay
PUT YOUR BEARD IN MY MOUTH
TVSTRANGERTHINGS
sheepfilms
I'd rather be in outer space 🛸
Alisa U Zemlji Chuda

⁂

JVL

@theartofmadeline

Product Placement
styofa doing anything

seen from Germany
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@sadstrawbrries
@daenerya secret gift exchange ❤ for @sardoniyx
» Destiny is something that we’ve invented because we can’t stand that fact that everything that happens is accidental.
↳ Sleepless in Seattle (1993) dir. Nora Ephron
Original caption: “Explore the majestic beauty of running through the Swiss Alps.”
Portrait Of An Enemy.
Lucia Heffernan
Art by suyou_kang
Fiona whose hobbies include chasing lizards, snuffling water, flooping and being ever curious.
A spider weaving its web. (Source)
spiny backed garden orb weaver spider, also known as the crab-like orbweaver and the spiny orb weaver.
Trying to draw buildings
yo here’s a useful tip from your fellow art ho cynellis… use google sketchup to create a model of the room/building/town you’re trying to draw… then take a screenshot & use it as a reference! It’s simple & fun!
Sketchup is incredibly helpful. I can’t recommend it enough.
There’s a 3D model warehouse where you can download all kinds of stuff so you don’t have to build everything from scratch.
reblog to save a life
This is an incomplete tutorial, and it drives me crazy every time I see it come around.
We live in a pretty great digital age and we have access to a ton of amazing tools that artists in past generations couldn’t even dream of, but a lot of people look at a cool trick and only learn half of the process of using it.
Here’s the missing part of this tutorial:
How do you populate your backgrounds?
Well, here’s the answer:
If the focus is the environment, you must show a person in relation to that environment.
The examples above are great because they show how to use the software itself, but each one just kind of “plops” the character in front of their finished product with no regard of the person’s relation to their environment.
How do you fix this?
Well, here’s the simplest solution:
This is a popular trick used by professional storyboard and comic artists alike when they’re quickly planning compositions. It’s simple and it requires you to do some planning before you sit down to crank out that polished, final version of your work, but it will be the difference between a background and an environment.
From Blacksad (artist: Juanjo Guarnido)
From Hellboy (Mike Mignola)
Even if your draftsmanship isn’t that great (like mine), people can be more immersed in the story you tell if you just make it feel like there is a world that exists completely separate from the one in which they currently reside – not just making a backdrop the characters stand in front of.
Your creations live in a unique world, and it is as much a character as any other member of the cast. Make it as believable as they are.
Great comments and tutorials!
I’m a 3d artist and have been exploring the possibilities of using 3d as reference for 2d poses. I want to add a couple of tips and things!
Sketchup is very useful for environment references, and I assume it’s reasonably easy to learn. If you’re interested in going above and beyond, I highly recommend learning a proper 3d modeling program to help with art, especially because you can very easily populate a scene or location with characters!
Using 3ds Max I can pretty quickly construct an environment for reference. But going beyond that, I can also pose a pretty simple ‘CAT’ armature (known in 3d as a rig) straight into the scene, which can be totally customized, from various limbs, tails, wings, whatever, to proportions, and also can be modeled onto and expanded upon (for an example, you could 3d sculpt a head reference for your character and then attach it to the CAT rig, so you have a reference for complex face angles!)
The armature can also be posed incredibly easily. I know programs exist for stuff like this - Manga Studio, Design Doll - but posing characters in these programs is always an exercise in frustration and very fiddly imo. A simple 3d rig is impossibly easy to pose.
By creating an environment and dropping my character rig into it, I have an excellent point of reference when it comes to drawing the scene!
Not only that, but I can also view the scene from whatever angle I could ever want or need, including the character and their pose/position relative to the environment.
We can even quickly and easily expand this scene to include more characters!
Proper 3d modeling software is immensely powerful, and if you wanted to, you could model a complex environment that occurs regularly in your comic or illustration work (say, a castle interior, or an outdoor forest environment) and populate the scene with as many perspective-grounded characters as you need!
reblogging to save a life
!!!!!!!!!!!!!!
Look at this amazing addition! This is fantastic!
Hi I love bees
2018-08-12
they say the best burn brightest when circumstances are at their worst
cutest little house
yo what are you always so stressed about?
me:
Was this the intention
very tired cat writing a term paper
Rodarte Spring 2019 RTW
Stars
Stars are the most widely recognized astronomical objects, and represent the most fundamental building blocks of galaxies. The age, distribution, and composition of the stars in a galaxy trace the history, dynamics, and evolution of that galaxy. Moreover, stars are responsible for the manufacture and distribution of heavy elements such as carbon, nitrogen, and oxygen, and their characteristics are intimately tied to the characteristics of the planetary systems that may coalesce about them. Consequently, the study of the birth, life, and death of stars is central to the field of astronomy.
How do stars form?
Stars are born within the clouds of dust and scattered throughout most galaxies. A familiar example of such as a dust cloud is the Orion Nebula.
Turbulence deep within these clouds gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction. As the cloud collapses, the material at the center begins to heat up. Known as a protostar, it is this hot core at the heart of the collapsing cloud that will one day become a star.
Three-dimensional computer models of star formation predict that the spinning clouds of collapsing gas and dust may break up into two or three blobs; this would explain why the majority the stars in the Milky Way are paired or in groups of multiple stars.
As the cloud collapses, a dense, hot core forms and begins gathering dust and gas. Not all of this material ends up as part of a star — the remaining dust can become planets, asteroids, or comets or may remain as dust.
In some cases, the cloud may not collapse at a steady pace. In January 2004, an amateur astronomer, James McNeil, discovered a small nebula that appeared unexpectedly near the nebula Messier 78, in the constellation of Orion. When observers around the world pointed their instruments at McNeil’s Nebula, they found something interesting — its brightness appears to vary. Observations with NASA’s Chandra X-ray Observatory provided a likely explanation: the interaction between the young star’s magnetic field and the surrounding gas causes episodic increases in brightness.
Main Sequence Stars
A star the size of our Sun requires about 50 million years to mature from the beginning of the collapse to adulthood. Our Sun will stay in this mature phase (on the main sequence as shown in the Hertzsprung-Russell Diagram) for approximately 10 billion years.
Stars are fueled by the nuclear fusion of hydrogen to form helium deep in their interiors. The outflow of energy from the central regions of the star provides the pressure necessary to keep the star from collapsing under its own weight, and the energy by which it shines.
As shown in the Hertzsprung-Russell Diagram, Main Sequence stars span a wide range of luminosities and colors, and can be classified according to those characteristics. The smallest stars, known as red dwarfs, may contain as little as 10% the mass of the Sun and emit only 0.01% as much energy, glowing feebly at temperatures between 3000-4000K. Despite their diminutive nature, red dwarfs are by far the most numerous stars in the Universe and have lifespans of tens of billions of years.
On the other hand, the most massive stars, known as hypergiants, may be 100 or more times more massive than the Sun, and have surface temperatures of more than 30,000 K. Hypergiants emit hundreds of thousands of times more energy than the Sun, but have lifetimes of only a few million years. Although extreme stars such as these are believed to have been common in the early Universe, today they are extremely rare - the entire Milky Way galaxy contains only a handful of hypergiants.
Stars and Their Fates
In general, the larger a star, the shorter its life, although all but the most massive stars live for billions of years. When a star has fused all the hydrogen in its core, nuclear reactions cease. Deprived of the energy production needed to support it, the core begins to collapse into itself and becomes much hotter. Hydrogen is still available outside the core, so hydrogen fusion continues in a shell surrounding the core. The increasingly hot core also pushes the outer layers of the star outward, causing them to expand and cool, transforming the star into a red giant.
If the star is sufficiently massive, the collapsing core may become hot enough to support more exotic nuclear reactions that consume helium and produce a variety of heavier elements up to iron. However, such reactions offer only a temporary reprieve. Gradually, the star’s internal nuclear fires become increasingly unstable - sometimes burning furiously, other times dying down. These variations cause the star to pulsate and throw off its outer layers, enshrouding itself in a cocoon of gas and dust. What happens next depends on the size of the core.
Average Stars Become White Dwarfs
For average stars like the Sun, the process of ejecting its outer layers continues until the stellar core is exposed. This dead, but still ferociously hot stellar cinder is called a White Dwarf. White dwarfs, which are roughly the size of our Earth despite containing the mass of a star, once puzzled astronomers - why didn’t they collapse further? What force supported the mass of the core? Quantum mechanics provided the explanation. Pressure from fast moving electrons keeps these stars from collapsing. The more massive the core, the denser the white dwarf that is formed. Thus, the smaller a white dwarf is in diameter, the larger it is in mass! These paradoxical stars are very common - our own Sun will be a white dwarf billions of years from now. White dwarfs are intrinsically very faint because they are so small and, lacking a source of energy production, they fade into oblivion as they gradually cool down. This fate awaits only those stars with a mass up to about 1.4 times the mass of our Sun. Above that mass, electron pressure cannot support the core against further collapse. Such stars suffer a different fate as described below.
Supernovae Leave Behind Neutron Stars or Black Holes
Main sequence stars over eight solar masses are destined to die in a titanic explosion called a supernova. A supernova is not merely a bigger nova. In a nova, only the star’s surface explodes. In a supernova, the star’s core collapses and then explodes. In massive stars, a complex series of nuclear reactions leads to the production of iron in the core. Having achieved iron, the star has wrung all the energy it can out of nuclear fusion - fusion reactions that form elements heavier than iron actually consume energy rather than produce it. The star no longer has any way to support its own mass, and the iron core collapses. In just a matter of seconds the core shrinks from roughly 5000 miles across to just a dozen, and the temperature spikes 100 billion degrees or more. The outer layers of the star initially begin to collapse along with the core, but rebound with the enormous release of energy and are thrown violently outward. Supernovae release an almost unimaginable amount of energy. For a period of days to weeks, a supernova may outshine an entire galaxy. Likewise, all the naturally occurring elements and a rich array of subatomic particles are produced in these explosions. On average, a supernova explosion occurs about once every hundred years in the typical galaxy. About 25 to 50 supernovae are discovered each year in other galaxies, but most are too far away to be seen without a telescope.
Neutron Stars
If the collapsing stellar core at the center of a supernova contains between about 1.4 and 3 solar masses, the collapse continues until electrons and protons combine to form neutrons, producing a neutron star. Neutron stars are incredibly dense - similar to the density of an atomic nucleus. Because it contains so much mass packed into such a small volume, the gravitation at the surface of a neutron star is immense.
Neutron stars also have powerful magnetic fields which can accelerate atomic particles around its magnetic poles producing powerful beams of radiation. Those beams sweep around like massive searchlight beams as the star rotates. If such a beam is oriented so that it periodically points toward the Earth, we observe it as regular pulses of radiation that occur whenever the magnetic pole sweeps past the line of sight. In this case, the neutron star is known as a pulsar.
Black Holes
If the collapsed stellar core is larger than three solar masses, it collapses completely to form a black hole: an infinitely dense object whose gravity is so strong that nothing can escape its immediate proximity, not even light. Since photons are what our instruments are designed to see, black holes can only be detected indirectly. Indirect observations are possible because the gravitational field of a black hole is so powerful that any nearby material - often the outer layers of a companion star - is caught up and dragged in. As matter spirals into a black hole, it forms a disk that is heated to enormous temperatures, emitting copious quantities of X-rays and Gamma-rays that indicate the presence of the underlying hidden companion.
From the Remains, New Stars Arise
The dust and debris left behind by novae and supernovae eventually blend with the surrounding interstellar gas and dust, enriching it with the heavy elements and chemical compounds produced during stellar death. Eventually, those materials are recycled, providing the building blocks for a new generation of stars and accompanying planetary systems.
Credit and reference: science.nasa.gov
image credit: ESO, NASA, ESA, Hubble