Hi! I have been thinking about Marc and the ways he expresses his anger... giving the cold shoulder... the silent treatment if you will (he will speak ABOUT vale but not TO vale let alone WITH vale)... need your input please....
hmm good question.... this got. STUPID long sorry
uhhh marc is, in general, good at keeping his (negative) emotions in check. like i think marc loooooves to think of himself on track as a mature, controlled, and rational dude. above distraction. a killer. a cyborg. idk his dad has talked about how he doesnt really complain much about injury and there's also allll these stories about what a mature kid he was... so i think that when he was young - ESPECIALLY in a racing sense because he was so much younger than most of the people he was competing against - he internalized that in order to do all the stuff he wants to do racing-wise, he reallyyyy has to keep a level head and not well. act his age! and i think that extends to a lot of how he manages his emotions today (at least in a public setting). even in places where im pretty sure hes PISSED (sepang. phillip island 2013.) he just kind of. visibly contains himself. not a confrontational dude in the outright sense he'll clench his jaw and try to work through it.
which is part of what makes his valentino-oriented crazy so interesting. bc people were noticing that marc in 2015 was kind of. being weird. as his and valentino's relationship deteriorated. like they were both outwardly very much like we can keep it on track :) until the big fallout towards the end of the year but uhhhh. well marc has said that vale started pulling back in september of 2014 like he was noticing SOMETHING, and they clashed on track A LOT in 2015, and i think marc sensed vale cooling on him and freaked a lil. hashtag neurotic 22 year old moments. he is my favorite crazy ex girlfriend. like usually he IS good at separating that stuff out and managing his emotions in the racing sense but in assen that year when vale overtook him off track after they made contact he raised a BIG stink with race direction and actually had some uh. not especially chill quotes about it. (it should be noted marc was also flopping for the first time in his motogp career. like in his brain he stopped winning AND vale stopped talking to him he was goin through it) adn all the reporters noticed too they were like. why werent you sucking and fucking in parc ferme. like vale's left turn wrt to spaniard sabotage comes outta nowhere but people WERE noticing that things were changing. i bet marc noticed too. BUT they are not the type of people to talk about these things so they keep it to vague flirting in presscons and escalating on-track tension slash proxy wars waged in race-direction contexts... liek truly you are 22 you are not going to keep your championship title and your hot sports idol bestie is no longer flirting with you on twitter and you COULD just talk to him about that but you'd rather DIE so youre going to ask honda to back you up to race direction about your last race where you DEFINITELY lost bc winning is the ONLY thing thatll make you feel better. even though thatll help convince your hot sports idol that you are engaging in a benedict arnold level betrayal scheme against him. an insane time to be marc marquez. 2015 really kind of is a study on how both of them handle losing: NOT WELL.
and then the thing about sepang is that then the lid is blown clean off and marc spends the ENTIRE race being annoying on purposeeeee. hes so fucking pissed and hurt at valentino that he decides to get under his skin for REALSIES instead of focusing on his race. like idk he probably would have fought hard for the win without the drama that how he works but uh. i think he was being annoying specifically to bite at vale's edges. and part of that is bc marc is naturally and effortlessly annoying. but i think part of it was SPITE. like his team advised him not to speak on anything from that presscon and he didnt, but he can still fuck him over on track. get under his skin. like he cant tell vale to his FACE that he's angry and confused and hurt. but he CAN let him know on that fucking racing line. where he cant be ignored. idk like i cant see marc letting anyone else get under his skin like that.
AND another big ass exception to the marc marquez anger management philosophy is from misano 2019 where vale messes with his qualifying lap. a lovely anon sent me some videos of marc talking to the press and jesus christ i dont think ive ever seen him angrier oh my god. AND the anon also linked the race from that weekend where he won and he celebrated harder than ive seen him celebrate some TITLE wins like he went. notably nuts. the commentators were all like uhhhh. he mustve REALLY wanted to get one over on vale adjfhlkdh... idk if any of this answered your question but his relationship to his emotions fascinates me hes so weirddddd. and its interesting to me that he can shrug off jorge ruining his last race at honda and be friendly but also be like. kind of aloofly pissed at bezz. because of valentino! he can repress the rest of it, but valentino shines through the cracks.
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You stated all my thoughts about White. Up until this point he has no stakes in this story. They better do something with his character quick because there are only three eps left and I could not care less about whether he lives or dies right now. I even want Fluke’s selfish crazy ass to survive more than White at this point.
they just aren't giving us anything about white. as far as we know, he's just boyfriend. he has no ties with non and has done nothing to harm him or the investigation. he just doesn't have many ties to the main story with non. let's be honest. it makes him a little boring and bland. i kinda care about him cause he seems nice. he's innocent. there's nothing wrong with his place in the story and i feel like he does have his seat at the table even if he's not involved with non. he plays detective with phee and tan and he does his best with trying to contact the outside world. we see how fluke is going crazy through how he interacts with white. we get to see tee fleshed out a little through white.
i just don't think it would be satisfying to leave him as final girl. i mean, it's just too cookie cutter to leave the "innocent" one alive. this doesn't really seem like a story that's so rigid in its sense of morality. a lot of the characters we see are very much not black and white. you have phee who cares very much for non, but sleeps with jin and, at least the way i see it, kind of likes him too. he's on his mission to seek the truth about non or kinda get revenge but he gets distracted and veers off course. we have tee who is a major bully and does fucked up things to non which could have landed him in jail and did land him into deep shit with his uncle, but he also ultimately asked for mercy for non and tee is dealing with a lot of shit at home. i mean, he has the health of his dad on his shoulders (if i remember correctly) and his uncle was stepping on his neck threatening him with money or the lack of it. i am a tee hater but when i really think of his situation, i can't help but feel bad for the guy and everything that he's going through. and i love phee, but man was it fucked up to sleep with jin without knowing the full story.
with all of these complex and interesting characters to really dig into and analyze, white just seems bland in comparison and i feel like that's probably the point of his character. i mean, maybe i just haven't caught onto any foreshadowing, but white isn't going to turn out to be some great mastermind or part of the conspiracy with phee and tan in the end. that would feel like such shitty writing. i think this is more or less confirmed by white getting the hallucination of boils on his skin. he's not in on the plan and he didn't use this to throw off suspicion like tan did.
i think he works best as a tragic death. he would work best as collateral in the end. he has done all that he can and that is still not enough sometimes. you can do all the right things but circumstances get you sometimes. that's just what life is.
white is not final girl material. this story ultimately isn't about him, and i think that's what seals his fate. no part of seeing him coming out of the woods bloody and crying would be satisfying as an ending and would honestly create the most basic ass theme. it would make me actually angry if the "innocent" one got out alive. in a show that works so hard at being morally complex, that is such a slap in the face as an ending. it sends the most basic theme of "if you do bad things, bad things happen to you, and if you do good things, good things happen to you." the story would say nothing interesting. it is such a tired theme that doesn't take into acount the cemplexities and nuances of life.
i believe dff will do better than that. i think it will give us a story that leaves all of us speechless and satisfied. white being the final girl will not give us that.
sorry anon that i unloaded all of this on you. i never really got into it in my original post, and i still didn't fully get into it here but this was getting long.
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For the Halsin "don't deserve to see the sun again" theme, if the player fails to break the Shadow Curse before starting act 3, when they say goodbye to Halsin in the Shadow-Cursed Lands, he says, "I will miss you, my friend. Perhaps our paths will cross again some day, if the sun ever shines on this place once more." So... more of Halsin viewing the sun as a reward of sorts, or at least the absence of light as the ultimate punishment
It's about...the cyclical balance of the Sun being the most powerful of lifebringers, as well as the most dangerous of killers. It's about wishing for nothing more than to see the light after eons of darkness, but it blinds and burns you as it's primary reward; and your body sings for it - it has sung for it since the dawn of all times. No matter the hardship to bask in its presence, it is still, in the end, a symbol of hope. And isn't it - for those brief moments of happiness it brings the spirit - worth the hardship for a chance to have it look upon you again?
Purple prose aside, as the Sun is a life bringer, and there were entire druidian rituals and worship surrounding the Sun, I'm not surprised many of Halsin's tidings of bad fortune in his mind is an absence of being able to reap its benefits - whether that be figuratively or literally is up to interpretation (I think it's a bit of both).
It's also worth noting how one of his main wishes is that *everyone* can see the Sun, at all levels and walks of life, and that it is something that should never be limited to one's "worth" in society. It is a right, not a privilege.
Which does make Orin's mocking: "I do not deserve to see the sun again." twist the knife a little deeper in the gut.
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from a doylist/logistical standpoint, i get why a lot of the fiddling with dimensions we get tends to stay within the set boundaries of a given iteration. just look how they massacred the 87!gang, especially in the 2012 xovers. heck, they just slapped together some new lore for 87!krang all retcon style!
but the idea of having a big reveal where a character already baked into a modern iteration turns out to be not just a counterpart of a previous version of the character, but that actual character themself, having traveled through dimensions to end up in the new iteration…you gotta admit, if it got done properly, it'd be so cool.
ope! this villain swore vengeance as their fancy schmancy machinery malfunctioned and seemingly vaporized everything? huh. well they look to be gone but we'll keep our eyes peeled for their return…except they never come back. maybe they were planned to return, maybe not. maybe there was time in the show/comic's run to address it, maybe it got cancelled before they got a chance. it just seems like a plot thread that never got properly taken care of.
smash cut to another iteration. the local version of the villain in question has been fairly close to the source material thus far, but they've been working on something In Secret™, eh? whoopsie-daisies, it's straight-up just the dude from before, slowly building their power back up! their new and improved evil plan is revealed: they intend on taking out the local turtles before plunging into the multiverse to return home and eliminate their turtles! MWAHAHAHAHA!
yes, it would probably be a nightmare to coordinate any returning VAs or to figure out how to account for VAs who maybe can't reprise their roles. yes, it would probably suck balls to try and do multiple artstyles justice at the same time, be they animated, comic book, or being brought from one to the other. yes, trying to balance two different turtleverses' "vibes" by striking a happy medium between the two without completely wrecking anybody's characterization would be (and clearly has been) notoriously difficult.
but man, that would be such a fun watch. and potentially even a good way for canon catharsis for the older iteration, if the villain in question was one the fans already liked.
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Astronomy 101: Stellar Life Cycles
This is the first in a series of posts I plan to make explaining basic astronomy concepts. I am not a professional astronomer, but I have a B.S. in Astronomy and Astrophysics, experience performing professional astronomical research (primarily photometry), and a lifelong amateur interest in astronomy. I am committed to accuracy in these posts (though some simplification is necessary) and welcome questions/comments.
(Image source)
Nearly every aspect of a star’s evolution is governed by a single characteristic: the star’s mass. Stellar masses are enormous, and so astronomers find it more convenient to measure them in solar masses (M☉, M being mass, and ☉ being the astronomical symbol for the sun, pronounced “M-sol”). 1 M☉ is equivalent to the sun’s mass; 2 M☉ is twice the sun’s mass; 0.5 M☉ is half the sun’s mass; and so on. Our sun masses approximately two quintillion kilograms—that’s 30 zeroes!—so it’s easy to see why this convention makes comparisons between stars easier.
Stars are composed primarily of hydrogen, with non-trivial amounts of helium (ex. our sun is about 74% hydrogen and 25% helium). They fuse the elements within themselves to produce an outward pressure from radiation that balances the inward pressure imposed by their own gravity (gravity wants to collapse the star; radiation keeps this from happening). The lowest stellar mass that can sustain a fusion reaction is theorized to be 0.08 M☉. It’s not physically possible for a star to be smaller than this. On the other end, the most massive stars range up to 250 M☉. (It should be noted that as the universe ages, stars are getting smaller; it is hypothesized that new stars cannot exceed 150 M☉.)
Stars are born from the gravitational collapse of giant molecular clouds (GMC), which are large, cold, and relatively dense pockets of interstellar gas. It’s theorized that several mechanisms can trigger GMC collapse, including the shock wave from nearby supernovae, collisions with other clouds, or passing through the spiral arm of a galaxy (which is denser than other areas). These all disrupt the balance within the cloud. As it collapses, it begins to fragment, forming individual stars. One GMC will produce numerous protostars.
The protostar phase lasts a relatively short time, about 500,000 years for stars the size of the sun. During this time, the protostar continues to accrete mass from the surrounding nebula (its own pocket of the GMC). Gravitational collapse is countered by gas pressure and magnetic pressure rather than by nuclear fusion as the protostar grows. Eventually, this is not sufficient and the protostar begins to collapse and enters a new phase: it reaches sufficient density to ignite nuclear fusion in its core, and becomes a proper star.
Initial fusion in the core fuses hydrogen into helium. It may seem counter-intuitive, but the lower a star’s mass, the slower it burns through its fuel and the longer it remains in this phase of its life. Massive stars are not only much hotter than small stars, but they need to produce more energy to stave off gravitational collapse. This causes them to burn through their supply of hydrogen very quickly. Very low mass stars born early in our universe have not existed long enough to burn through their hydrogen supplies. Models predict stars of 0.1 M☉ will take 6-12 TRILLION years to exhaust their hydrogen, and our universe is only 13.8 billion years old. These stars are barely getting started. These stars, known as red dwarfs, will never become red giants. Instead, they will continuously mix their original hydrogen stores with their newly produced helium until the entire star is composed of helium, at which point fusion will shut down. As they reach the end, they are predicted to become blue dwarfs, and then eventually white dwarfs. No blue dwarfs presently exist because the universe is still young.
Stars more like our sun, ranging from 0.6 to 8 M☉, have lives more consistent with what many people are taught in high school science classes. When these stars exhaust the hydrogen in their core, they still contain a large volume of hydrogen in their outer layers. They enter the subgiant phase, where they fuse hydrogen in a shell surrounding the helium core, and the star begins to expand and cool. This new helium adds to the volume of the core, the hydrogen-fusing shell moves outwards. This phase lasts several million to two billion years, again with lower-mass stars spending longer in this phase.
(You may have read that the sun will get hotter as it ages. This is true, and it’s due to the fact that as the fraction of hydrogen in the core decreases, the core temperature and rate of fusion increase. The sun will contract and become hotter as it approaches the subgiant phase. It’s theorized that this will make the Earth uninhabitable in about one billion years. However, the effects of plate tectonics and specifically the subduction of water from the oceans and the gradual slowing of tectonic activity is likely to play as large a role if not larger.)
This hydrogen-burning shell supports the star against gravitational collapse until the helium core grows too large. The core will contract, and the outer layers will further expand and cool as the star becomes a red giant. In the case of our sun, its radius will expand beyond the orbit of the Earth, in about six billion years. Shell burning continues at an increasing rate, but the star is no longer in equilibrium, and the core continues to contract even as it increases in mass, until eventually the star begins fusing helium into carbon. This can happen very suddenly for stars at the lower end of this mass range, or more gradually for more massive stars. The growth of the star can also temporarily create new habitable zones, primarily for the moons of gas giants, lasting several hundred million years.
Stars in this mass range do not have sufficient mass to fuse carbon, and so when the helium is largely consumed in the core, the core begins to collapse, and this time, only a strange state of matter called electron degeneracy will stop it. The Pauli Exclusion principle states that no two electrons can occupy identical states, and electron degeneracy occurs when a star has collapsed to the point that all the electrons of the star have been forced to occupy all the lowest-available energy states within the atomic structure of the star. The energy of the gravitational collapse is insufficient to overcome this electron pressure. White dwarfs are very small and incomprehensibly dense; similar to the mass of the sun, they are similar in size to the Earth. A teaspoon of white dwarf would weigh about 15 tons. Fusion has ceased, and the star is an inert ball of slowly cooling degenerate matter.
This is the end of the road for stars in this mass range, which is most of the stars that presently exist in the universe. Very, very slowly, solo white dwarfs will continue to cool. White dwarfs are predicted to outlast the lifespan of galaxies as structures in our universe. They may still be extant when enough time has passed for proton decay to become a significant force and ultimately devour the white dwarf. If proton decay takes significantly longer than predicted or turns out to not exist, the ultimate fate of a white dwarf is to be devoured by a black hole in the very, very, very far future of our universe when other forms of stars have all ceased to exist. (The black hole era is predicted to begin 10^43 years after the Big Bang, but it’s dependent on a lot of poorly-understood factors. Safe to say, this is not anything anyone needs to worry about.)
More massive stars have a more interesting if shorter life. They blow through their hydrogen quickly, ranging from 1 billion years to as few as 10,000 years. (You can calculate here.) As these stars enter their supergiant phase, they lose mass rapidly due to strong stellar winds. These stars do possess enough mass for more complex fusion reactions, and will gradually develop shells fusing various elements, and finally in the core, ultimately producing iron via fusion. All elements aside from hydrogen, some helium, and small amounts of lithium and beryllium are created by stellar nuclear fusion. Iron, however, is special, because it is the lightest element on the periodic table that requires more energy to fuse than it produces through fusion. A star attempting to fuse iron is going into an energy deficit, rather than producing energy through radiation that can stave off gravitational collapse. A star cannot fuse iron.
The final days of such stars come on quickly. The core turns to iron within a few hundred years, so rapidly that there is little change in the outward appearance of the star, which continues shell burning right up to the end. Eventually, this iron core reaches the effective Chandrasekhar mass, a little larger than the mass of our sun, and the core can no longer support itself. The core collapses.
It’s easy to say the star then explodes in a supernova, but the truth is more complicated. A supernova is triggered by the release of gravitational potential energy from the core collapse. If this is insufficient, instead the core becomes a neutron star or a black hole with very little fanfare. Some supernovae (pair-instability supernova) do not leave behind any stellar remnant despite originating from supermassive stars. Other supernovae do not involve supermassive stars, but white dwarfs in binary pairs accreting matter from their stellar companion.
The core collapse takes less than a quarter of a second. Within a few hours, the shockwave reaches the surface of the star, which will brighten tremendously over the next few months. At peak, supernovae can outshine their host galaxies. Perhaps the most famous supernova, SN 1987A, was visible to the naked eye and wasn’t even located in our own galaxy, but in a satellite galaxy. This shockwave is incredibly high-energy, to the point that it not only ejects outer material from the star, but ignites fusion reactions in that material. Here, we have an excess of energy, and nuclear fusion reactions that require more energy than they create are possible. This is how all elements heavier than iron are created.
The core becomes a neutron star or a black hole. Which depends on a large number of variables, perhaps strangely only two of which are core mass and stellar mass. A neutron star is similar to a white dwarf, in that it is composed of degenerate matter, but in this case electron degeneracy was not strong enough and it is held up by neutron degeneracy. In this state, electrons have combined with protons to produce neutrons, leaving behind a highly dense star composed of nuclear matter. While a neutron star is again slightly more massive than our sun, it has a diameter of only about 20 kilometers. A teaspoon of neutron star weights approximately 4 billion tons. Many neutron stars rotate rapidly, giving off jets of radiation from their poles. These stars are known as pulsars. The fate of neutron stars is similar to that of white dwarfs; they will eventually merge into black holes in the far distant future.
Other stars become black holes. In this case, even neutron degeneracy cannot stave off gravitational collapse, and the core collapses into a singularity. A singularity is a poorly-understood object where spacetime curvature becomes infinite. We can study singularities mathematically, but we can’t observe one, because it is hidden behind an event horizon—a boundary surrounding the black hole where gravity is too strong for even light to escape. And if light can’t escape, we can’t observe anything inside the event horizon. Our current understand of physics also breaks down here; our theories of gravity aren’t sufficient to fully understand singularities. We can, however, study event horizons, accretion disks (matter falling into the black hole), and jets of particles and radiation some black holes exhibit. This has given us a good understanding of the external properties and behavior of black holes, and we detect them based on these characteristics and the effects they have on other objects (ex. an orbiting companion star).
So if everything eventually becomes part of a black hole, what happens to a black hole? The answer is they evaporate through a process called Hawking radiation. Essentially, according to quantum mechanics, space has a quality called vacuum energy that causes virtual particle pairs to continuously pop in and out of existence. The pair consists of one particle and one anti-particle, which annihilate each other and return the energy of their creation to the vacuum. Therefore, no energy is created or destroyed. However, every so often, one of these pairs pops into existence with one particle on the outer side of the event horizon, able to escape, and the other trapped inside the event horizon. The virtual particle that escapes becomes a real particle, and that energy has to come from somewhere. It takes it from the black hole. Because mass and energy are functionally equivalent, this drains a tiny amount of mass from the black hole. (Please note: this is a dramatic oversimplification, but gets the basic idea across.) On long enough timelines, this will cause even the largest of black holes to evaporate. Unlike just about everything else involving stars, smaller black holes evaporate more quickly than large ones.
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