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Star formation near the Sun is driven by expansion of the Local Bubble – Nature.com

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Abstract

For decades we have known that the Sun lies within the Local Bubble, a cavity of low-density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust1,2,3. However, the precise shape and extent of this shell4,5, the impetus and timescale for its formation6,7, and its relationship to nearby star formation8 have remained uncertain, largely due to low-resolution models of the local interstellar medium. Here we report an analysis of the three-dimensional positions, shapes and motions of dense gas and young stars within 200 pc of the Sun, using new spatial9,10,11 and dynamical constraints12. We find that nearly all of the star-forming complexes in the solar vicinity lie on the surface of the Local Bubble and that their young stars show outward expansion mainly perpendicular to the bubble’s surface. Tracebacks of these young stars’ motions support a picture in which the origin of the Local Bubble was a burst of stellar birth and then death (supernovae) taking place near the bubble’s centre beginning approximately 14 Myr ago. The expansion of the Local Bubble created by the supernovae swept up the ambient interstellar medium into an extended shell that has now fragmented and collapsed into the most prominent nearby molecular clouds, in turn providing robust observational support for the theory of supernova-driven star formation.

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Fig. 1: A 3D spatial view of the solar neighbourhood.
Fig. 2: The evolution of the Local Bubble and sequential star formation at the surface of its expanding shell.

Data availability

The datasets generated and/or analysed during the current study are publicly available on the Harvard Dataverse (https://dataverse.harvard.edu/dataverse/local_bubble_star_formation/), including Extended Data Table 1 (https://doi.org/10.7910/DVN/ZU97QD), Extended Data Table 2 (https://doi.org/10.7910/DVN/1VT8BC), per-star data for individual stellar cluster members (https://doi.org/10.7910/DVN/1UPMDX) and the cluster tracebacks (https://doi.org/10.7910/DVN/E8PQOD).

Code availability

The results generated in this work are based on publicly available software packages and do not involve the extensive use of custom code. Given each star’s reported Gaia data, we use the astropy38 package to obtain the Heliocentric Galactic Cartesian positions and velocities. The extreme deconvolution algorithm in the astroML51 package is used to estimate the mean 3D positions and velocities of the stellar clusters. The Orbit functionality in the galpy40 package is used to perform the dynamical tracebacks. The dynesty43 package is used to fit the analytic superbubble expansion model and determine the best-fit parameters governing the Local Bubble’s evolution.

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Acknowledgements

The visualization, exploration and interpretation of data presented in this work were made possible using the glue visualization software, supported under NSF grant numbers OAC-1739657 and CDS&E:AAG-1908419. The interactive figures were made possible by the plot.ly python library. D.P.F. acknowledges support by NSF grant AST-1614941 ‘Exploring the Galaxy: 3-Dimensional Structure and Stellar Streams’. D.P.F., A.A.G. and C.Z. acknowledge support by NASA ADAP grant 80NSSC21K0634 ‘Knitting Together the Milky Way: An Integrated Model of the Galaxy’s Stars, Gas, and Dust’. A.B. acknowledges support by the Excellence Cluster ORIGINS, which is funded by the German Research Foundation (DFG) under Germany’s Excellence Strategy -EXC-2094-390783311. J.A. acknowledges support from the Data Science Research Centre and the TURIS Research Platform of the University of Vienna. J.G. acknowledges funding by the Austrian Research Promotion Agency (FFG) under project number 873708. C.Z. acknowledges that support for this work was provided by NASA through the NASA Hubble Fellowship grant number HST-HF2-51498.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. C.Z., A.A.G., J.A. and S.B. acknowledge Interstellar Institute’s program ‘The Grand Cascade’ and the Paris-Saclay University’s Institut Pascal for hosting discussions that encouraged the development of the ideas behind this work.

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C.Z. led the work and wrote the majority of the text. All authors contributed to the text. C.Z., A.A.G. and J.A. led interpretation of the observational results, aided by S.B., M.F. and A.B. who helped interpret their significance in light of theoretical models for supernova-driven star formation. C.Z. and A.A.G. led the visualization efforts. J.S.S. and D.P.F. helped shape the statistical modelling of the Local Bubble’s expansion. C.Z., A.A.G. and J.S.S. contributed to the software used in this work. J.G. and C.S. provided data for and the subsequent interpretation of the 3D kinematics of the Orion region. D.K. helped to develop the code used to model the 3D positions and motions of stellar clusters described in the Methods.

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Catherine Zucker.

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Extended data figures and tables

Extended Data Fig. 1 1D and 2D marginal distributions (“corner plot”) of the model parameters governing the evolution of the Local Bubble’s expanding shell.

Parameters include the time since the first explosion (i.e. the age of the Local Bubble), texp, the density of the ambient medium the bubble is expanding into, n0, the time between supernova explosions powering its growth, 𝞓tSNe, and the thickness/uncertainty on the expanding shell radius 𝞓R. In the 1D distributions, the vertical dashed lines denote the median and 1𝝈 errors, while in the 2D distributions, we show the 0.5𝝈, 1𝝈, 1.5𝝈, and 2𝝈 contours.

Extended Data Fig. 2 Temporal evolution of the Local Bubble, based on the fit to the dynamical tracebacks and the analytic expansion model22 summarized in the Methods section.

Panel a) The evolution of the Local Bubble’s expansion velocity vexp. Panel b) The evolution of the Local Bubble’s shell radius Rshell. Panel c) The evolution of the average momentum injection per supernova . The thick purple line represents the median fit, while the thin purple lines represent random samples. We estimate a current radius of (165pm 6) pc and current expansion velocity of (6,.7,_-0.4^+0.5) km/s, corresponding to time t=0 Myr (the present day).

Extended Data Fig. 3 PDF of the estimate of the number of supernovae required to power the Local Bubble’s expansion.

The estimate is obtained by comparing the shell’s present-day momentum to the average momentum injected by supernovae.

Extended Data Fig. 4 Analysis of the stellar tracebacks of the UCL and LCC clusters, whose progenitors were likely responsible for the supernovae that created the Local Bubble.

The scatter points indicate the positions of the current cluster members of UCL and LCC, which are colored as a function of time (spanning the present day in pink to 30 Myr ago in black). Panel a: Using Hipparcos data and adopting a solar peculiar motion (U, V, W) = (10.0, 5.2, 7.2) km/s46, previous literature6,7 find that UCL and LCC were born outside the Local Bubble (black trace4) 15 Myr ago and only entered its present-day boundary in the past 5 Myr (reproduced from Fig. 6 in ref. 6). Panel b: We attempt to reproduce the results from previous literature6,7 using the same data and solar motion, but are unable to account for the curvature of the tracebacks, finding the UCL and LCC formed just inside its northern boundary 15 Myr ago. Panel c: Using a different value for the solar motion, (U, V, W) = (10.0, 15.4, 7.8) km/s41 but the same Hipparcos data, we find that UCL and LCC were born near the center of the Local Bubble. Panel d: Finally, using updated Gaia data but the same adopted solar motion used in panel c. (U, V, W) = (10.0, 15.4, 7.8) km/s41, we also find that UCL and LCC were born near the center of the bubble, given an updated model for its surface13.

Extended Data Table 1 Summary of the 3D positions and 3D velocities of young stellar clusters within 400 pc of the Sun
Extended Data Table 2 Temporal evolution of cluster births at the surface of the Local Bubble’s expanding shell

Supplementary information

Peer Review File

Supplementary Figure 1

Interactive 3D visualization of dense gas and young stars on the Local Bubble’s surface. This figure is the interactive 3D counterpart to Fig. 1. The figure supports interactive panning, zooming and rotation. Individual data layers can be toggled on/off by clicking on the layer in the legend on the right-hand side of the figure. The surface of the Local Bubble13 is shown in purple. The short squiggly coloured lines (or ‘skeletons’) demarcate the 3D spatial morphology of dense gas in prominent nearby molecular clouds11. The 3D cones indicate the positions of young stellar clusters, with the apex of the cone pointing in the direction of stellar motion. The Sun is marked with a yellow cross. We also overlay the morphology of the 3D dust (grey blobby shapes9) and the models for two Galactic scale features—the Radcliffe Wave (red)16 and the Split (blue)10. The Per-Tau Superbubble15 (green sphere) is also overlaid.

Supplementary Figure 2

Interactive 3D visualization of the Local Bubble’s expansion. This figure is the interactive 3D counterpart to Fig. 2. The figure supports interactive panning, zooming and rotation. Individual data layers can be toggled on/off by clicking on the layer in the legend on the right-hand side of the figure. Stellar cluster tracebacks are shown with the coloured paths. Before the cluster birth, the tracebacks are shown as semi-transparent circles meant to guide the eye, since our modelling is insensitive to the dynamics of the gas before its conversion into stars. After the cluster birth, the tracebacks are shown with filled circles and terminate in a large dot, which marks the cluster’s current position. For time snapshots ≤14 Myr ago, we overlay a model for the evolution of the Local Bubble (purple sphere), as derived in the Methods. Click ‘Play Forward’ to see the Local Bubble evolve starting 17 Myr ago and progressing forwards to the present day. Click ‘Play Backward’ to see the evolution in reverse. Click ‘Pause’ to stop the animation. Alternatively, drag the time slider back and forth to view the Local Bubble’s expansion at any time. To jump to epochs of particular interest, click on any of the ‘action’ buttons (for example, ‘UCL Born’) on the right-hand side of the figure.

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Zucker, C., Goodman, A.A., Alves, J. et al. Star formation near the Sun is driven by expansion of the Local Bubble.
Nature (2022). https://doi.org/10.1038/s41586-021-04286-5

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  • Received: 18 August 2021

  • Accepted: 26 November 2021

  • Published: 12 January 2022

  • DOI: https://doi.org/10.1038/s41586-021-04286-5

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Here’s how Helene and other storms dumped a whopping 40 trillion gallons of rain on the South

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More than 40 trillion gallons of rain drenched the Southeast United States in the last week from Hurricane Helene and a run-of-the-mill rainstorm that sloshed in ahead of it — an unheard of amount of water that has stunned experts.

That’s enough to fill the Dallas Cowboys’ stadium 51,000 times, or Lake Tahoe just once. If it was concentrated just on the state of North Carolina that much water would be 3.5 feet deep (more than 1 meter). It’s enough to fill more than 60 million Olympic-size swimming pools.

“That’s an astronomical amount of precipitation,” said Ed Clark, head of the National Oceanic and Atmospheric Administration’s National Water Center in Tuscaloosa, Alabama. “I have not seen something in my 25 years of working at the weather service that is this geographically large of an extent and the sheer volume of water that fell from the sky.”

The flood damage from the rain is apocalyptic, meteorologists said. More than 100 people are dead, according to officials.

Private meteorologist Ryan Maue, a former NOAA chief scientist, calculated the amount of rain, using precipitation measurements made in 2.5-mile-by-2.5 mile grids as measured by satellites and ground observations. He came up with 40 trillion gallons through Sunday for the eastern United States, with 20 trillion gallons of that hitting just Georgia, Tennessee, the Carolinas and Florida from Hurricane Helene.

Clark did the calculations independently and said the 40 trillion gallon figure (151 trillion liters) is about right and, if anything, conservative. Maue said maybe 1 to 2 trillion more gallons of rain had fallen, much if it in Virginia, since his calculations.

Clark, who spends much of his work on issues of shrinking western water supplies, said to put the amount of rain in perspective, it’s more than twice the combined amount of water stored by two key Colorado River basin reservoirs: Lake Powell and Lake Mead.

Several meteorologists said this was a combination of two, maybe three storm systems. Before Helene struck, rain had fallen heavily for days because a low pressure system had “cut off” from the jet stream — which moves weather systems along west to east — and stalled over the Southeast. That funneled plenty of warm water from the Gulf of Mexico. And a storm that fell just short of named status parked along North Carolina’s Atlantic coast, dumping as much as 20 inches of rain, said North Carolina state climatologist Kathie Dello.

Then add Helene, one of the largest storms in the last couple decades and one that held plenty of rain because it was young and moved fast before it hit the Appalachians, said University of Albany hurricane expert Kristen Corbosiero.

“It was not just a perfect storm, but it was a combination of multiple storms that that led to the enormous amount of rain,” Maue said. “That collected at high elevation, we’re talking 3,000 to 6000 feet. And when you drop trillions of gallons on a mountain, that has to go down.”

The fact that these storms hit the mountains made everything worse, and not just because of runoff. The interaction between the mountains and the storm systems wrings more moisture out of the air, Clark, Maue and Corbosiero said.

North Carolina weather officials said their top measurement total was 31.33 inches in the tiny town of Busick. Mount Mitchell also got more than 2 feet of rainfall.

Before 2017’s Hurricane Harvey, “I said to our colleagues, you know, I never thought in my career that we would measure rainfall in feet,” Clark said. “And after Harvey, Florence, the more isolated events in eastern Kentucky, portions of South Dakota. We’re seeing events year in and year out where we are measuring rainfall in feet.”

Storms are getting wetter as the climate change s, said Corbosiero and Dello. A basic law of physics says the air holds nearly 4% more moisture for every degree Fahrenheit warmer (7% for every degree Celsius) and the world has warmed more than 2 degrees (1.2 degrees Celsius) since pre-industrial times.

Corbosiero said meteorologists are vigorously debating how much of Helene is due to worsening climate change and how much is random.

For Dello, the “fingerprints of climate change” were clear.

“We’ve seen tropical storm impacts in western North Carolina. But these storms are wetter and these storms are warmer. And there would have been a time when a tropical storm would have been heading toward North Carolina and would have caused some rain and some damage, but not apocalyptic destruction. ”

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‘Big Sam’: Paleontologists unearth giant skull of Pachyrhinosaurus in Alberta

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It’s a dinosaur that roamed Alberta’s badlands more than 70 million years ago, sporting a big, bumpy, bony head the size of a baby elephant.

On Wednesday, paleontologists near Grande Prairie pulled its 272-kilogram skull from the ground.

They call it “Big Sam.”

The adult Pachyrhinosaurus is the second plant-eating dinosaur to be unearthed from a dense bonebed belonging to a herd that died together on the edge of a valley that now sits 450 kilometres northwest of Edmonton.

It didn’t die alone.

“We have hundreds of juvenile bones in the bonebed, so we know that there are many babies and some adults among all of the big adults,” Emily Bamforth, a paleontologist with the nearby Philip J. Currie Dinosaur Museum, said in an interview on the way to the dig site.

She described the horned Pachyrhinosaurus as “the smaller, older cousin of the triceratops.”

“This species of dinosaur is endemic to the Grand Prairie area, so it’s found here and nowhere else in the world. They are … kind of about the size of an Indian elephant and a rhino,” she added.

The head alone, she said, is about the size of a baby elephant.

The discovery was a long time coming.

The bonebed was first discovered by a high school teacher out for a walk about 50 years ago. It took the teacher a decade to get anyone from southern Alberta to come to take a look.

“At the time, sort of in the ’70s and ’80s, paleontology in northern Alberta was virtually unknown,” said Bamforth.

When paleontogists eventually got to the site, Bamforth said, they learned “it’s actually one of the densest dinosaur bonebeds in North America.”

“It contains about 100 to 300 bones per square metre,” she said.

Paleontologists have been at the site sporadically ever since, combing through bones belonging to turtles, dinosaurs and lizards. Sixteen years ago, they discovered a large skull of an approximately 30-year-old Pachyrhinosaurus, which is now at the museum.

About a year ago, they found the second adult: Big Sam.

Bamforth said both dinosaurs are believed to have been the elders in the herd.

“Their distinguishing feature is that, instead of having a horn on their nose like a triceratops, they had this big, bony bump called a boss. And they have big, bony bumps over their eyes as well,” she said.

“It makes them look a little strange. It’s the one dinosaur that if you find it, it’s the only possible thing it can be.”

The genders of the two adults are unknown.

Bamforth said the extraction was difficult because Big Sam was intertwined in a cluster of about 300 other bones.

The skull was found upside down, “as if the animal was lying on its back,” but was well preserved, she said.

She said the excavation process involved putting plaster on the skull and wooden planks around if for stability. From there, it was lifted out — very carefully — with a crane, and was to be shipped on a trolley to the museum for study.

“I have extracted skulls in the past. This is probably the biggest one I’ve ever done though,” said Bamforth.

“It’s pretty exciting.”

This report by The Canadian Press was first published Sept. 25, 2024.

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The ancient jar smashed by a 4-year-old is back on display at an Israeli museum after repair

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TEL AVIV, Israel (AP) — A rare Bronze-Era jar accidentally smashed by a 4-year-old visiting a museum was back on display Wednesday after restoration experts were able to carefully piece the artifact back together.

Last month, a family from northern Israel was visiting the museum when their youngest son tipped over the jar, which smashed into pieces.

Alex Geller, the boy’s father, said his son — the youngest of three — is exceptionally curious, and that the moment he heard the crash, “please let that not be my child” was the first thought that raced through his head.

The jar has been on display at the Hecht Museum in Haifa for 35 years. It was one of the only containers of its size and from that period still complete when it was discovered.

The Bronze Age jar is one of many artifacts exhibited out in the open, part of the Hecht Museum’s vision of letting visitors explore history without glass barriers, said Inbal Rivlin, the director of the museum, which is associated with Haifa University in northern Israel.

It was likely used to hold wine or oil, and dates back to between 2200 and 1500 B.C.

Rivlin and the museum decided to turn the moment, which captured international attention, into a teaching moment, inviting the Geller family back for a special visit and hands-on activity to illustrate the restoration process.

Rivlin added that the incident provided a welcome distraction from the ongoing war in Gaza. “Well, he’s just a kid. So I think that somehow it touches the heart of the people in Israel and around the world,“ said Rivlin.

Roee Shafir, a restoration expert at the museum, said the repairs would be fairly simple, as the pieces were from a single, complete jar. Archaeologists often face the more daunting task of sifting through piles of shards from multiple objects and trying to piece them together.

Experts used 3D technology, hi-resolution videos, and special glue to painstakingly reconstruct the large jar.

Less than two weeks after it broke, the jar went back on display at the museum. The gluing process left small hairline cracks, and a few pieces are missing, but the jar’s impressive size remains.

The only noticeable difference in the exhibit was a new sign reading “please don’t touch.”

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