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Scientists Spot a Solar Flare With Surprising Spectral Behavior
On August 19, 2022, solar astronomers using the Daniel K. Inouye Solar Telescope (DKIST) on the Hawaiian island of Maui caught the fading remnants of a C-class solar flare. Their observations showed something unusual: very strong spectral fingerprints of calcium II H and hydrogen-epsilon lines. It was the first time these two light signatures were seen in great detail during the decline of a solar flare. According to computer models, those lines were stronger than expected and play a not well-understood role in how flares heat the solar atmosphere where they occur. The same models can be used to study flares in other stars, as well.
Spectra are produced when the light from an object, in this case, the Sun, passes through a specialized instrument that breaks the light into its component wavelengths. The light can be emitted, absorbed, or reflected. Solar flares always provide interesting spectral lines, and this one was no different. In the case of the flare on August 19th, light was emitted by energized molecules of calcium II H and hydrogen-epsilon. These two are close together in the solar spectrum and provide a window into what’s happening in the solar chromosphere. That’s the complex layer of the solar atmosphere between the visible surface (photosphere) and corona (outer atmosphere). These absorption lines indicate ionized calcium in the atmosphere, and are clues to chromospheric activity and the strength of magnetic fields in the regions where they exist.
A visible image of the Sun on August 19, 2022, showing sunspots and their active regions, including 3078 where the DKIST observed unusual spectral lines. Courtesy CESAR Helios Observatory.
It hasn’t always been easy to study these spectral lines in solar flares from Earth, usually due to constraints on telescope time and instrumentation. The DKIST was able to capture these thanks to its high-resolution capabilities. The lines in the August 2022 studies not only surprised the observers, but also revealed weaknesses in their models of solar physics. When the science team led by student observer Cole Tamburri compared the observations with current computer models that simulate how flares are heated, they found that their models could reproduce some features, but failed to fully explain others. The observed light signatures were broader and differed in brightness in ways the models can’t yet explain, particularly as they showed up when the flare was declining. Apparently, there are more complex physics at work that computer simulations of the complex physics of a flare don’t quite take into account. Data from these observations will be used to strengthen the models for future use.
How a Solar Flare Unfolds
To understand the surprise in the spectra during the flare’s decline, let’s take a look at how a solar flare works from start to finish. First, there’s a precursor stage. That’s when the local magnetic fields over an active region get entangled, like twisted rubber bands. This phase shows soft x-ray emissions. As the fields get more twisted, the flare progresses to the impulsive (explosive) stage. That’s where the magnetic fields break and release strong amounts of stored energy in the form of high-energy protons and electrons are accelerated and speed away from the Sun. This stage also shows intense x-ray emissions, gamma rays, and radio waves. The flare brightens in response. Eventually, the flare begins to decline and this decay stage sees the flare’s energy levels start to settle down and the region cools down. That’s what the models tell scientists to expect. Current models suggest that the heating during a flare happens either by beams of high-energy particles or by heat spreading through the solar atmosphere.
This sequences shows the evolution of a bright flare ribbon using the Visible Broadband Imager on the Daniel K. Inouye Solar Telescope. The flare occurred in active region 13078. Credit: Tamburri, et al.
The team originally had hoped to use DKIST to capture the precursor, “ramp-up” stage of this C6.7-class flare. Instead, they captured the end stage, when activity and emissions were declining. Their observations showed spectral lines for the calcium II H and hydrogen-epsilon emissions that didn’t match what was expected for the declining stage of a flare. That told the scientists that the flare’s emissions stayed stronger and more complex than they expected even as the flare cooled and decayed.
Reality vs. Models
The surprising observational data, made using the DKIST Visible Spectropolarimeter (ViSP) and the Visible Broadband Imager, gave the team a high-cadence, high-resolution set of spectra and provided simultaneous, high-resolution imaging needed to reveal the physical structure of the flare itself. “Both ground-based, high-resolution observing and state-of-the-art flare modeling are incredibly complex,” said Tamburri, who noted that a large team of scientists was required to make observations and analyze the data. “The combined expertise from many NSO scientists in both regimes made this work possible. Collaboration of this type is essential to solving the remaining questions in flare physics using both modern observations and models.”
(a) A comparison of a RADYN+RH simulated Ca II H and H lines to observations made by the Daniel K. Inouye Solar Telescope.. (b) A comparison of ViSP observations to the modeled H profiles that are notably in emission in panel (a), using in the input RH atmosphere file. Note also the locations of several other lines within the spectral range of H, from Fe I, Fe I, and Ni I. The two Fe I lines in the red wing are deeper in the quiet Sun than the flare spectra, giving the impression of an emission line when the pre-flare is subtracted. Intensity values include pre-flare subtraction and are normalized to the maximum intensity of H in order to easily compare the widths of observed and modeled lines. The observed line profiles from ViSP at ribbon center at 20:42:07 UT are shown in black. This is a figure from a paper describing the observations (see references below). Courtesy Tamburri, et al.
Team members compared the emissions data they obtained from DKIST with current theoretical physics models for flares, using a computational model called RADYN. It simulates how the solar atmosphere gets heated by flare activity. It turned out that the data agreed with some parts of the models but not others. For example, the physical models actually agreed with the data regarding the shape and width of the hydrogen-epsilon line. However, the models didn’t exactly match the calcium II H line shape. The light signatures were very different from what the models suggested. That leaves a big gap to explain how flares heat the solar atmosphere.
The NSO researchers behind the study say improving these models will require rethinking how flare heating works. More observations during solar flare events using DKIST should help strengthen the current models of solar atmospheric heating. In particular, they should be able to use detailed observations of the impulsive (explosive) and cooling phases to test new ideas about how flares behave through all the phases of their activity.
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Why now? Because that’s how trauma works. Get over it

Why now? Why now?
Every time a woman comes forward with her story of sexual assault, this is the first question she faces. OK, maybe the second — after some variation of “Are you a lying slut?”
At least we are consistent. But on behalf of all survivors everywhere, of any gender, identity or age, let me give you some blanket answers to “Why now?”
Survivors come forward now, whenever now is, because they have reached the point in their recovery when facing the inevitable “lying slut” accusation is less terrible than watching their abuser strut around as if that person is not a dangerous, cruel predator who is almost certainly going to hurt someone else if they are not stopped.
Whether it’s in Congress, on a movie set, in the halls of their school — wherever that predator is just living their life without consequence — there is a survivor who has been cowering in the shadows of her own life, in pain, wanting to scream to the world that this person is not what they seem.
But the price of that honesty has always been steep. Too steep. Even after #MeToo.
Ask Cassie Ventura. Ask Jennifer Siebel Newsom. Ask E. Jean Carroll. Dolores Huerta. Simone Biles.
Even powerful women can’t escape the blowback, the fear. Even powerful women are steamrolled over and over again by the overwhelming presumption that they are lying, and there is an ulterior motive for coming forward at this particular moment.
Imagine just being an average person holding that secret. Who are any of us to stand up alone against a rich and powerful man whose very freedom will depend on crushing our credibility?
P. Diddy. Harvey Weinstein. Donald Trump. Cesar Chavez. Larry Nassar. Eric Swalwell.
Those men know power, and know how to use it.
“He thought he was untouchable. He acted with total impunity. He never thought that the consequences of his actions would follow him,” Ally Sammarco, one of the women who has spoken out about Swalwell (who has previously denied allegations of misconduct), told CBS.
It’s why the women of the Epstein files stayed silent for so long. It’s why there are thousands of rape survivors out there right now who have never said a word about what they endured, and maybe never will.
“Why now?” is just a more palatable version of “lying slut,” a question based on ignorance about how trauma — and society — works. A question meant not to elicit fact, but to feed the Jezebel frenzy men always use in their attempt to escape justice.
Here’s the truth about sexual assault: There is no right way to respond to it, no right time. There is no one reaction that proves it happened or that creates the perfect scenario that will protect the survivor’s reputation while delivering justice upon the predator. In fact, there is really no way at all to respond to a sexual assault that won’t bring secondary trauma.
Wait years and face disdain — that it didn’t happen, wasn’t serious, is only coming out now for some agenda, like politics or money.
Report it immediately and be prepared for every move, every smile, every sip of a drink, to be examined for signs that this was, if not consensual, somehow deserved — a gray area of shared responsibility.
Imagine, at a moment of crushing vulnerability, when your body has been violated and your mind is reeling trying to find safe ground, being bludgeoned by these accusations, stated or implied, that you brought this on yourself.
“Why now?” becomes “Why would you?”
Even when the scenario is one in which there can be no defense — such as the UCLA gynecologist, James Heaps, who on Tuesday pleaded guilty to sexually abusing five of his patients during exams — the cost of reporting is terrible. That case has wound on for years, leaving each of the victims to constantly relive their worst moments, constantly fear that all of their courage would come to nothing.
Which is why survivors don’t always come forward. Maybe they need time to put themselves back together, even just a little bit. Maybe the fear of all that societal scrutiny is just too much. Maybe they fear they won’t be believed, and their attacker will be free to harm them again.
Maybe they just want it to all go away. Maybe they do blame themselves, and are paralyzed by an unfounded shame.
There are so many reasons why survivors stay silent — and none of them are because it didn’t happen, or because they are lying.
Lonna Drewes, the Beverly Hills model who came forward Tuesday with an accusation that Swalwell drugged and raped her in 2018, summed up the experience of many, many survivors.
“I did not want to live anymore,” she said of how she felt after the attack. “I cried all the time for years.”
So here’s the real answer to “Why now?” from a victim’s statement that one of Heap’s survivors read in court.
“What you intended to break, you did not,” she said.
That is the answer to “Why now?” Because the bravery and courage at the heart of the survivor was bruised but not defeated.
Because she doesn’t want it to happen to anyone else.
Because she deserves to be free of his secrets: Ones she has been forced to keep out of fear of him, but also of us.
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Middle East War Will Slow Global Economic Growth, I.M.F. Warns
The conflict could also fuel another bout of inflation, according to the International Monetary Fund.
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Are Neutrinos Their Own Evil Twins? Part 3: Dirac’s Direct Solution
(This is Part 3 of a series on neutrinos, Majorana fermions, and one of the strangest open questions in physics. Read Part 1 and Part 2.)
Neutrinos have mass. We know this. And massive particles — ALL massive particles, as we established in Part 1 — flicker between left- and right-handed states. That flickering IS the mass. The constant Higgs handshake, the endless switching. That’s the deal. That’s what makes it all hang together.
But neutrinos don’t flicker. Left-handed neutrinos stay left-handed. Right-handed antineutrinos stay right-handed. No switching. No flickering. Nothing. And yet they have mass.
So either everything we just said about mass is wrong — and I’m pretty confident it isn’t — or something very strange is going on with the neutrino.
The most straightforward solution is this: the right-handed neutrinos ARE there. They exist. We just can’t see them.
Here’s why that works. Think about the electron. The electron has two completely independent ways to describe it. One: handedness. Left or right. But we’ve found that for a massive particle this is just the flickering — transient, constantly changing. It’s not a permanent label. Handedness for an electron is almost…incidental. It doesn’t define what the electron fundamentally IS.
But there’s another way to describe an electron: particle versus antiparticle. Electron versus positron. And THIS one is permanent. Important. Pinned open by electric charge. An electron has charge. A positron has the opposite. If they meet, they annihilate in a flash of pure energy. The universe treats this distinction as sacred, because charge is conserved, and the universe does not mess around with conserved quantities.
So for the electron: handedness flickers and doesn’t really matter. Particle versus antiparticle is locked and fundamental and really, REALLY matters. Two descriptions. One important, one not.
This gives us what we can reasonably call the Dirac picture — named after Paul Adrien Maurice Dirac, who first worked out the mathematics of relativistic quantum particles. In this picture, the neutrino works exactly the same way as the electron. Two options for handedness, two options for charge. Four total combinations.
Left-handed neutrino: we see them, the weak force loves them. Right-handed antineutrino: we see them too, the weak force produces them in beta decay. Those are the observable ones.
Then there are the other two. Right-handed neutrino. Left-handed antineutrino. These exist in the theory. They just don’t interact with anything. Our germaphobic weak force won’t touch them — wrong hands, remember? They have no electric charge, so electromagnetism ignores them. No color charge, so the strong force ignores them. The only force they EVER feel is gravity. They are, in the most complete and total sense imaginable, invisible. Not hard to detect. Not rare. Not shy. INVISIBLE. Completely, permanently, in-principle undetectable by any instrument we could ever conceivably build.
They could be in this room RIGHT NOW and we have no way of detecting them.
And look — it works. The math is consistent. It explains why we only see left-handed neutrinos.
There’s even something genuinely beautiful hiding in it. If those right-handed neutrinos exist and are ENORMOUSLY massive — and I mean absurdly, almost comically massive, like ten to the fifteen times heavier than a proton — then something elegant falls out of the mathematics. Their mass and the mass of ordinary left-handed neutrinos end up inversely linked. Make the right-handed partner heavier, and the left-handed neutrino gets lighter. It’s called the seesaw mechanism. Push one end down, the other goes up. And it would explain why neutrino masses are so vanishingly, almost insultingly tiny. The lightness of the neutrino would be a direct echo of the enormousness of something we can never directly observe.
That’s nice.
But here’s the thing. When it comes to the electron, its two descriptions — handedness and particle-versus-antiparticle — are kept independent by electric charge. Charge is what forces them apart. Charge is what insists that “electron” and “positron” are categorically different things that cannot be confused or collapsed into each other.
But the neutrino has no electric charge. We have bookkeeping devices that keep neutrinos distinct from antineutrinos in our equations — but unlike electric charge, they’re not sacred. They’re not protected by any deep principle. They’re accidental. The universe didn’t mandate those rules. They just fell out of the math, because we designed the math that way.
Here’s the thing: nothing is FORCING the distinction between “neutrino” and “antineutrino” to be fundamental.
And that’s the crack in the door that Ettore Majorana walked through.
In Part 4, we get to Majorana’s last paper — and the experiment that might finally answer the question he left behind.
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