NEW: The Highest-Energy Cosmic Rays Originate From Unknown Galaxies

Where do cosmic rays come from? Solving a 50-year old mystery, a collaboration of researchers has discovered it is much farther than the Milky Way.

In an paper published in the scientific journal ‘Science’, the Pierre Auger Collaboration has definitively answered the question of whether cosmic particles had originated from outside the Milky Way Galaxy. Their research notes that studying the distribution of the cosmic ray arrival directions is the first step in determining where the extragalactic particles originate.

The collaborating scientists were able to make their recordings using the largest cosmic ray observatory ever built, the Pierre Auger Observatory in Argentina. Included in this collaboration are David Nitz and Brian Fick, professors of physics at Michigan Technological University.

“We are now considerably closer to solving the mystery of where and how these extraordinary particles are created, a question of great interest to astrophysicists,” says Karl-Heinz Kampert, a professor at the University of Wuppertal in Germany and spokesperson for the Auger Collaboration, which involves more than 400 scientists from 18 countries.

Cosmic rays are the nuclei of elements from hydrogen to iron. Studying them gives scientists a way to study matter from outside our solar system – and now, outside our galaxy. Cosmic rays help us understand the composition of galaxies and the processes that occur to accelerate the nuclei to nearly the speed of light. By studying cosmic rays, scientists may come to understand what mechanisms create the nuclei.

To put it simply, understanding cosmic rays and where they originate can help us answer fundamental questions about the origins of the universe, our galaxy and ourselves.



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JUST IN: New NASA Mission Explores ‘Cosmic Rain’

A new experiment set for an Aug. 14 launch to the International Space Station will provide an unprecedented look at a rain of particles from deep space, called cosmic rays, that constantly showers our planet. The Cosmic Ray Energetics And Mass mission destined for the International Space Station (ISS-CREAM) is designed to measure the highest-energy particles of any detector yet flown in space.

Cosmic Ray Energetics And Mass

The ISS-CREAM experiment will be delivered to the space station as part of the 12th SpaceX commercial resupply service mission. Once there, ISS-CREAM will be moved to the Exposed Facility platform extending from Kibo, the Japanese Experiment Module. “High-energy cosmic rays carry a great deal of information about our interstellar neighborhood and our galaxy, but we haven’t been able to read these messages very clearly,” said co-investigator John Mitchell at Goddard. “ISS-CREAM represents one significant step in this direction.”

At energies above about 1 billion electron volts, most cosmic rays come to us from beyond our solar system. Various lines of evidence, including observations from NASA’s Fermi Gamma-ray Space Telescope, support the idea that shock waves from the expanding debris of stars that exploded as supernovas accelerate cosmic rays up to energies of 1,000 trillion electron volts (PeV). That’s 10 million times the energy of medical proton beams used to treat cancer. ISS-CREAM data will allow scientists to examine how sources other than supernova remnants contribute to the population of cosmic rays.

Protons are the most common cosmic ray particles, but electrons, helium nuclei and the nuclei of heavier elements make up a small percentage. All are direct samples of matter from interstellar space. But because the particles are electrically charged, they interact with galactic magnetic fields, causing them to wander in their journey to Earth. This scrambles their paths and makes it impossible to trace cosmic ray particles back to their sources.

BREAKING NEWS: New Study Suggests Electric Discharge Between Earth’s Core and Magnetic Field

This news release highlights the observation of charged particles in the form of what is sometimes described as “sprites”, which is an electrical discharge which surges from “below” to “above”. It is similar to the mechanics of a local lightening/thunderstorm we witness here on Earth. To the typical observer, it appears that lightening comes down from the heavens and strikes the Earth; however, it is the intense impulse of charge which comes from the ground which produces high voltage.

The existence of these upper atmosphere sprites has been reported by pilots for years sparking a healthy debate as to their cause and how they exist. ESA astronaut Andreas Mogensen during his mission on the International Space Station in 2015 was asked to take pictures over thunderstorms with the most sensitive camera on the orbiting outpost to look for these brief features.

Denmark’s National Space Institute has now published the results of photos taken by ESA astronaut Andreas Mogensen, of upper atmosphere discharges, sometimes referred to as blue lightening or ‘sprites’. The video taken by Mogensen were from the (ISS) International Space Station. (shown below)

The cause or effects of these charged particle events are not well understood. Researched data does suggest a connection between Earth’s magnetic field and Earth’s core. With this hypothesis as a foundation, my personal research suggest a continued conjunction goes beyond our Heliosphere and into our galaxy Milky Way.

The blue discharges and jets are examples of a little-understood part of our atmosphere called the heliosphere. The Heliosphere is the outer atmosphere of the Sun and marks the edge of the Sun’s magnetic influence in space. The solar wind that streams out in all directions from the rotating Sun is a magnetic plasma, and it fills the vast space between the planets in our solar system.

The magnetic plasma from the Sun does not conjoin with the magnetic plasma between the stars in our galaxy, allowing the solar wind carves out a bubble-like atmosphere that shields our solar system from the majority of galactic cosmic rays.

Andreas concludes, “It is not every day that you get to capture a new weather phenomenon on film, so I am very pleased with the result – but even more so that researchers will be able to investigate these intriguing thunderstorms in more detail soon.”

New Space Weather Model Helps Simulate Magnetic Structure of Solar Storms

The dynamic space environment that surrounds Earth – the space our astronauts and spacecraft travel through – can be rattled by huge solar eruptions from the Sun, which spew giant clouds of magnetic energy and plasma, a hot gas of electrically charged particles, out into space. The magnetic field of these solar eruptions are difficult to predict and can interact with Earth’s magnetic fields, causing space weather effects.


A new tool called EEGGL – short for the Eruptive Event Generator (Gibson and Low) and pronounced “eagle” – helps map out the paths of these magnetically structured clouds, called coronal mass ejections or CMEs, before they reach Earth. EEGGL is part of a much larger new model of the corona, the Sun’s outer atmosphere, and interplanetary space, developed by a team at the University of Michigan. Built to simulate solar storms, EEGGL helps NASA study how a CME might travel through space to Earth and what magnetic configuration it will have when it arrives. The model is hosted by the Community Coordinated Modeling Center, or CCMC, at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.

The new model is known as a “first principles” model because its calculations are based on the fundamental physics theory that describes the event – in this case, the plasma properties and magnetic free energy, or electromagnetics, guiding a CME’s movement through space.

Such computer models can help researchers better understand how the Sun will affect near-Earth space, and potentially improve our ability to predict space weather, as is done by the U.S. National Oceanic and Atmospheric Administration.

Taking into account the magnetic structure of a CME from its initiation at the Sun could mark a big step in CME modeling; various other models initiate CMEs solely based on the kinematic properties, that is, the mass and initial velocity inferred from spacecraft observations. Incorporating the magnetic properties at CME initiation may give scientists a better idea of a CME’s magnetic structure and ultimately, how this structure influences the CME’s path through space and interaction with Earth’s magnetic fields – an important piece to the puzzle of the Sun’s dynamic behavior.

The model begins with real spacecraft observations of a CME, including the eruption’s initial speed and location on the Sun, and then projects how the CME could travel based on the fundamental laws of electromagnetics. Ultimately, it returns a series of synthetic images, which look similar to those produced of actual observations from NASA and ESA’s SOHO or NASA’s STEREO, simulating the CME’s propagation through space.

A team led by Tamas Gombosi at the University of Michigan’s Department of Climate and Space Sciences and Engineering developed the model as part of its Space Weather Modeling Framework, which is also hosted at the CCMC. All of the CCMC’s space weather models are available for use and study by researchers and the public through runs on request. In addition, EEGGL, and the model it supports, is the first “first principles” model to simulate CMEs including their magnetic structure open to the public.

BREAKING NEWS: New Discovery of Ancient Tree Rings Indicate Stable Predictable Sunspot Cycle Over 300 Million Years Period

I know your first instinct is to say something like “duh”. I would certainly support you in this analysis. However, setting this obvious notion aside, this new finding does attribute a great amount of credibility to the scientific discipline of cycles; furthermore, it provides a greater comprehension in regards to ‘time-linked’ measurements such as short-term, medium-term  and long-term cycles. Examples would be the 11 year sunspot cycle, the 26,000 year precession cycle, and the Milankovitch or Eccentricity cycle with a 100,000 and 410,000 cycle.

In a new study published in the scientific journal Geology, researchers Ludwig Luthardt, professor at the Natural History Museum in Chemnitz, and Ronald Rößler, professor at Freiberg University of Mining and Technology, describe how they found evidence in ancient tree rings, identifying a solar sunspot cycle that occurred millions of years ago and compared it to recent cycles . “The median tree-ring curve of that period revealed a 10.62 year cycle, the duration of which is almost identical to the modern 11 year solar cycle we see today,” said Luthardt.

Sunspot activity swings between a period known as ‘solar maximum’, at which time an enormous amount of radiation is released through the development of powerful streams of charged particles which is released in various forms such as solar flares, coronal mass ejections, coronal holes, and purging filaments.

When a percentage of these particles penetrate the Earth’s magnetic field and continue into the upper and lower atmosphere, the measured effects are captured in assorted forms of Flora such as tree-rings, lake bottom sediment, and deep ice cores. Such high-resolution records are commonly used for reconstructing climatic variations in the younger geological history.

The team discovered large wooded tree trunks from the early Permian Fossil Forest of Chemnitz, southeast Germany. This region had been covered by lava during a volcanic eruption during the Permian period, offering a historical record of Sun activity. “For the first time we applied dendrochronological methods (tree-ring dating) – to Paleozoic trees in order to recognize annual variations; says Rößler.

The team found that sunspot activity recorded 300 million years ago as reflected in tree ring archived analysis, matches almost identically with today’s caused fluctuations of cosmic radiation input to the atmosphere.


NASA Study Finds Solar Storms Could Spark Soils at Moon’s Poles

Powerful solar storms can charge up the soil in frigid, permanently shadowed regions near the lunar poles, and may possibly produce “sparks” that could vaporize and melt the soil, perhaps as much as meteoroid impacts, according to NASA-funded research. This alteration may become evident when analyzing future samples from these regions that could hold the key to understanding the history of the moon and solar system.

The moon has almost no atmosphere, so its surface is exposed to the harsh space environment. Impacts from small meteoroids constantly churn or “garden” the top layer of the dust and rock, called regolith, on the moon. “About 10 percent of this gardened layer has been melted or vaporized by meteoroid impacts,” said Andrew Jordan of the University of New Hampshire, Durham. “We found that in the moon’s permanently shadowed regions, sparks from solar storms could melt or vaporize a similar percentage.” Jordan is lead author of a paper on this research published online in Icarus August 31, 2016.

Explosive solar activity, like flares and coronal mass ejections, blasts highly energetic, electrically charged particles into space. Earth’s atmosphere shields us from most of this radiation, but on the moon, these particles—ions and electrons—slam directly into the surface. They accumulate in two layers beneath the surface; the bulky ions can’t penetrate deeply because they are more likely to hit atoms in the regolith, so they form a layer closer to the surface while the tiny electrons slip through and form a deeper layer. The ions have positive charge while the electrons carry negative charge. Since opposite charges attract, normally these charges flow towards each other and balance out.

In August 2014, however, Jordan’s team published simulation results predicting that strong solar storms would cause the regolith in the moon’s permanently shadowed regions (PSRs) to accumulate charge in these two layers until explosively released, like a miniature lightning strike. The PSRs are so frigid that regolith becomes an extremely poor conductor of electricity. Therefore, during intense solar storms, the regolith is expected to dissipate the build-up of charge too slowly to avoid the destructive effects of a sudden electric discharge, called dielectric breakdown. The research estimates the extent that this process can alter the regolith.

“This process isn’t completely new to space science electrostatic discharges can occur in any poorly conducting (dielectric) material exposed to intense space radiation, and is actually the leading cause of spacecraft anomalies,” said Timothy Stubbs of NASA’s Goddard Space Flight Center in Greenbelt, Maryland, a co-author of the paper. The team’s analysis was based on this experience. From spacecraft studies and analysis of samples from NASA’s Apollo lunar missions, the researchers knew how often large solar storms occur. From previous lunar research, they estimated that the top millimeter of regolith would be buried by meteoroid impacts after about a million years, so it would be too deep to be subject to electric charging during solar storms. Then they estimated the energy that would be deposited over a million years by both meteoroid impacts and dielectric breakdown driven by solar storms, and found that each process releases enough energy to alter the regolith by a similar amount.

“Lab experiments show that dielectric breakdown is an explosive process on a tiny scale,” said Jordan. “During breakdown, channels could be melted and vaporized through the grains of soil. Some of the grains may even be blown apart by the tiny explosion. The PSRs are important locations on the moon, because they contain clues to the moon’s history, such as the role that easily vaporized material like water has played. But to decipher that history, we need to know in what ways PSRs are not pristine; that is, how they have been weathered by the space environment, including solar storms and meteoroid impacts.”

The next step is to search for evidence of dielectric breakdown in PSRs and determine if it could happen in other areas on the moon. Observations from NASA’s Lunar Reconnaissance Orbiter spacecraft indicate that the soil in PSRs is more porous or “fluffy” than other areas, which might be expected if breakdown was blasting apart some of the soil grains there. However, experiments, some already underway, are needed to confirm that breakdown is responsible for this. Also, the lunar night is long—about two weeks—so it can become cold enough for breakdown to occur in other areas on the moon, according to the team. There may even be “sparked” material in the Apollo samples, but the difficulty would be determining if this material was altered by breakdown or a meteoroid impact. The team is working with scientists at the Johns Hopkins University Applied Physics Laboratory on experiments to see how breakdown affects the regolith and to look for any tell-tale signatures that could distinguish it from the effects of meteoroid impacts.