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.


BREAKING NEWS: A New Powerful Study Affirms Battros 2012 Equation

When Earth overheats, it finds its way to maintain its ambient temperature. In very much the same way humans sweat through our pores to cool off, in like manner, Earth sweats by producing increased mantle plume activity.

New research released this week confirms increased heat from Earth’s core strengthens the flow viscous material (liquefied rock) upward through the mantle having an effect on tectonic plates, including seamounts which in-turn heats the oceans.

For decades, scientists have theorized that the movement of Earth’s tectonic plates is driven largely by negative buoyancy created as they cool. New research, however, shows plate dynamics are driven significantly by the additional force of heat drawn from the Earth’s core.

The new findings also challenge the theory that underwater mountain ranges known as mid-ocean ridges are passive boundaries between moving plates. The findings show the East Pacific Rise, the Earth’s dominant mid-ocean ridge, is dynamic as heat is transferred.

David B. Rowley, professor of geophysical sciences at the University of Chicago, and fellow researchers came to the conclusions by combining observations of the East Pacific Rise with insights from modeling of the mantle flow there. The findings were published Dec. 23 in Science Advances.

“We see strong support for significant deep mantle contributions of heat-to-plate dynamics in the Pacific hemisphere,” said Rowley, lead author of the paper. “Heat from the base of the mantle contributes significantly to the strength of the flow of heat in the mantle and to the resultant plate tectonics.”

The researchers estimate up to approximately 50 percent of plate dynamics are driven by heat from the Earth’s core and as much as 20 terawatts of heat flow between the core and the mantle.

Unlike most other mid-ocean ridges, the East Pacific Rise as a whole has not moved east-west for 50 to 80 million years, even as parts of it have been spreading asymmetrically. These dynamics cannot be explained solely by the subduction of a process whereby one plate moves under another or sinks. Researchers in the new findings attribute the phenomena to buoyancy created by heat arising from deep in the Earth’s interior.

“The East Pacific Rise is stable because the flow arising from the deep mantle has captured it,” Rowley said. “This stability is directly linked to and controlled by mantle upwelling,” or the release of heat from Earth’s core through the mantle to the surface.

The Mid-Atlantic Ridge, particularly in the South Atlantic, also may have direct coupling with deep mantle flow, he added.

“The consequences of this research are very important for all scientists working on the dynamics of the Earth, including plate tectonics, seismic activity and volcanism,” said Jean Braun of the German Research Centre for Geosciences, who was not involved in the research.

The forces at work

Convection, or the flow of mantle material transporting heat, drives plate tectonics. As envisioned in the current research, heating at the base of the mantle reduces the density of the material, giving it buoyancy and causing it to rise through the mantle and couple with the overlying plates adjacent to the East Pacific Rise. The deep mantle-derived buoyancy, together with plate cooling at the surface, creates negative buoyancy that together explain the observations along the East Pacific Rise and surrounding Pacific subduction zones.

A debate about the origin of the driving forces of plate tectonics dates back to the early 1970s. Scientists have asked: Does the buoyancy that drives plates primarily derive from plate cooling at the surface, analogous with cooling and overturning of lakes in the winter? Or, is there also a source of positive buoyancy arising from heat at the base of the mantle associated with heat extracted from the core and, if so, how much does it contribute to plate motions? The latter theory is analogous to cooking oatmeal: Heat at the bottom causes the oatmeal to rise, and heat loss along the top surface cools the oatmeal, causing it to sink.

Until now, most assessments have favored the first scenario, with little or no contribution from buoyancy arising from heat at the base. The new findings suggest that the second scenario is required to account for the observations, and that there is an approximately equal contribution from both sources of the buoyancy driving the plates, at least in the Pacific basin.

“Based on our models of mantle convection, the mantle may be removing as much as half of Earth’s total convective heat budget from the core,” Rowley said.

Much work has been performed over the past four decades to represent mantle convection by computer simulation. Now the models will have to be revised to account for mantle upwelling, according to the researchers.

“The implication of our work is that textbooks will need to be rewritten,” Rowley said.

The research could have broader implications for understanding the formation of the Earth, Braun said. “It has important consequences for the thermal budget of the Earth and the so-called ‘secular cooling’ of the core. If heat coming from the core is more important than we thought, this implies that the total heat originally stored in the core is much larger than we thought.

“Also, the magnetic field of the Earth is generated by flow in the liquid core, so the findings of Rowley and co-authors are likely to have implications for our understanding of the existence, character and amplitude of the Earth’s magnetic field and its evolution through geological time,” Braun added.

ANNOUNCEMENT: Mitch Battros Guest On ‘The Conspiracy Show’ with Richard Syrett

Join me this Sunday (Jan. 22nd) for my guest appearance on Richard Syrett’s Conspiracy Show. Our focus will be on the latest news and research concerning the coming full magnetic pole shift. In addition, we will discuss the latest research on the cause of cyclical climate change the Earth has seen its whole life.

We will certainly touch on the Sun-Earth connection, but we will go much further than this to show newly found intricacies between our solar system and galaxy identifying cyclical expansions and contractions – which I might suggest mirrors that of a living entity in the way of “inhaling” and exhaling”. Showtime is 11 PM eastern – 8 PM pacific.
Radio Stations – Click Here

New Study Identifies Distinctive Emission Signatures of Pulsars

In two studies, international teams of astronomers suggest that recent images from NASA’s Chandra X-ray Observatory of two pulsars – Geminga and B0355+54 – may help shine a light on the distinctive emission signatures of pulsars, as well as their often perplexing geometry.

Pulsars are a type of neutron star that are born in supernova explosions when massive stars collapse. Discovered initially by lighthouse-like beams of radio emission, more recent research has found that energetic pulsars also produce beams of high energy gamma rays..

Interestingly, the beams rarely match up, said Bettina Posselt, senior research associate in astronomy and astrophysics, Penn State. The shapes of observed radio and gamma-ray pulses are often quite different and some of the objects show only one type of pulse or the other. These differences have generated debate about the pulsar model.

“It’s not fully understood why there are variations between different pulsars,” said Posselt. “One of the main ideas here is that pulse differences have a lot to do with geometry – and it also depends on how the pulsar’s spin and magnetic axes are oriented with respect to line of sight whether you see certain pulsars or not, as well as how you see them.”

Chandra’s images are giving the astronomers a closer than ever look at the distinctive geometry of the charged particle winds radiating in X-ray and other wavelengths from the objects, according to Posselt. Pulsars rhythmically rotate as they rocket through space at speeds reaching hundreds of kilometers a second. Pulsar wind nebulae (PWN) are produced when the energetic particles streaming from pulsars shoot along the stars’ magnetic fields, form tori – donut-shaped rings – around the pulsar’s equatorial plane, and jet along the spin axis, often sweeping back into long tails as the pulsars’ quickly cut through the interstellar medium.

“This is one of the nicest results of our larger study of pulsar wind nebulae,” said Roger W. Romani, professor of physics at Stanford University and principal investigator of the Chandra PWN project. “By making the 3-D structure of these winds visible, we have shown how one can trace back to the plasma injected by the pulsar at the center. Chandra’s fantastic X-ray acuity was essential for this study, so we are happy that it was possible to get the deep exposures that made these faint structures visible.”

A spectacular PWN is seen around the Geminga pulsar. Geminga – one of the closest pulsars at only 800 light years away from Earth – has three unusual tails, said Posselt. The streams of particles spewing out of the alleged poles of Geminga – or lateral tails – stretch out for more than half a light year, longer than 1,000 times the distance between the Sun and Pluto. Another shorter tail also emanates from the pulsar.

The astronomers said that a much different PWN picture is seen in the X-ray image of another pulsar called B0355+54, which is about 3,300 light years away from Earth. The tail of this pulsar has a cap of emission, followed by a narrow double tail that extends almost five light years away from the star.

While Geminga shows pulses in the gamma ray spectrum, but is radio quiet, B0355+54 is one of the brightest radio pulsars, but fails to show gamma rays.

“The tails seem to tell us why that is,” said Posselt, adding that the pulsars’ spin axis and magnetic axis orientations influence what emissions are seen on Earth.

According to Posselt, Geminga may have magnetic poles quite close to the top and bottom of the object, and nearly aligned spin poles, much like Earth. One of the magnetic poles of B0355+54 could directly face the Earth. Because the radio emission occurs near the site of the magnetic poles, the radio waves may point along the direction of the jets, she said. Gamma-ray emission, on the other hand, is produced at higher altitudes in a larger region, allowing the respective pulses to sweep larger areas of the sky.

“For Geminga, we view the bright gamma ray pulses and the edge of the pulsar wind nebula torus, but the radio beams near the jets point off to the sides and remain unseen,” Posselt said.

The strongly bent lateral tails offer the astronomers clues to the geometry of the pulsar, which could be compared to either jet contrails soaring into space, or to a bow shock similar to the shockwave created by a bullet as it is shot through the air.

Oleg Kargaltsev, assistant professor of physics, George Washington University, who worked on the study on B0355+54, said that the orientation of B0355+54 plays a role in how astronomers see the pulsar, as well. The study is available online in arXiv.

“For B0355+54, a jet points nearly at us so we detect the bright radio pulses while most of the gamma-ray emission is directed in the plane of the sky and misses the Earth,” said Kargaltsev. “This implies that the pulsar’s spin axis direction is close to our line-of-sight direction and that the pulsar is moving nearly perpendicularly to its spin axis.”

Noel Klingler, a graduate research assistant in physics, George Washington University, and lead author of the B0355+54 paper, added that the angles between the three vectors – the spin axis, the line-of-sight, and the velocity – are different for different pulsars, thus affecting the appearances of their nebulae.

“In particular, it may be tricky to detect a PWN from a pulsar moving close to the line-of-sight and having a small angle between the spin axis and our line-of-sight,” said Klingler.

In the bow-shock interpretation of the Geminga X-ray data, Geminga’s two long tails and their unusual spectrum may suggest that the particles are accelerated to nearly the speed of light through a process called Fermi acceleration. The Fermi acceleration takes place at the intersection of a pulsar wind and the interstellar material, according to the researchers, who report their findings on Geminga in the current issue of Astrophysical Journal.

Although different interpretations remain on the table for Geminga’s geometry, Posselt said that Chandra’s images of the pulsar are helping astrophysicists use pulsars as particle physics laboratories. Studying the objects gives astrophysicists a chance to investigate particle physics in conditions that would be impossible to replicate in a particle accelerator on earth.

“In both scenarios, Geminga provides exciting new constraints on the acceleration physics in pulsar wind nebulae and their interaction with the surrounding interstellar matter,” she said.

ALMA Starts Observing the Sun – VIDEO

Astronomers have harnessed ALMA‘s capabilities to image the millimeter-wavelength light emitted by the Sun’s chromosphere – the region that lies just above the photosphere, which forms the visible surface of the Sun. The solar campaign team, an international group of astronomers with members from Europe, North America and East Asia, produced the images as a demonstration of ALMA’s ability to study solar activity at longer wavelengths of light than are typically available to solar observatories on Earth.   Atacama Large Millimeter/submillimeter Array (ALMA)

Astronomers have studied the Sun and probed its dynamic surface and energetic atmosphere in many ways through the centuries. But, to achieve a fuller understanding, astronomers need to study it across the entire electromagnetic spectrum, including the millimeter and submillimeter portion that ALMA can observe.


Since the Sun is many billions of times brighter than the faint objects ALMA typically observes, the ALMA antennas were specially designed to allow them to image the Sun in exquisite detail using the technique of radio interferometry – and avoid damage from the intense heat of the focused sunlight. The result of this work is a series of images that demonstrate ALMA’s unique vision and ability to study our Sun.The data from the solar observing campaign are being released this week to the worldwide astronomical community for further study and analysis.

The team observed an enormous sunspot at wavelengths of 1.25 millimeters and 3 millimeters using two of ALMA’s receiver bands. The images reveal differences in temperature between parts of the Sun’s chromosphere. Understanding the heating and dynamics of the chromosphere are key areas of research that will be addressed in the future using ALMA.Sunspots are transient features that occur in regions where the Sun’s magnetic field is extremely concentrated and powerful. They are lower in temperature than the surrounding regions, which is why they appear relatively dark.

The difference in appearance between the two images is due to the different wavelengths of emitted light being observed. Observations at shorter wavelengths are able to probe deeper into the Sun, meaning the 1.25 millimeter images show a layer of the chromosphere that is deeper, and therefore closer to the photosphere, than those made at a wavelength of 3 millimeters.

ALMA is the first facility where ESO is a partner that allows astronomers to study the nearest star, our own Sun. All other existing and past ESO facilities need to be protected from the intense solar radiation to avoid damage. The new ALMA capabilities will expand the ESO community to include solar astronomers.

Asymmetric Structure in Supermassive Black Hole at Milky Way’s Center

The supermassive black hole candidate at the center of our Galaxy (associated with the radio source Sagittarius A*) is a prime candidate for studying the physical phenomena associated with accretion on to a supermassive black hole.

Sgr A* is thought to accrete at an extremely low rate; analogous situations in X-ray binary stars suggest that a jet may be present, making it challenging to formulate a fully self-consistent model that simultaneously explains its spectrum, its variability, its size and its shape.

Because Sgr A* is by far the closest supermassive black hole, its expected angular size (the shadow cast from its event horizon) is the largest of any known black hole candidate, making it a prime target for studies using very long baseline interferometry at mm wavelengths, which are capable of reaching spatial resolutions comparable to the expected shadow size.

CfA astronomer Shep Doeleman was a member of a team of twenty-two astronomers that used a combination of three widely separated millimeter telescope facilities, the Very Long Baseline Array, the Robert C. Byrd Green Bank Telescope, and the Large Millimeter Telescope Alfonso Serrano, to try to image the Sgr A* shadow. Their observations were taken in May of 2015 over the course of one evening, and the data from all the telescopes were analyzed to ascertain the geometry.

The scientists found some evidence for an asymmetric shape – a tiny extension that seems to protrude only a few AU from the central source (one astronomical unit is the average distance of the Earth from the Sun). This preliminary result could be due to scattering of the radiation by interstellar material, but it might also be associated with the black hole. Other observers have reported spotting some similar asymmetries, but the picture remains uncertain. The new result is a step forward, however, and future observations will try to refine and extend the current conclusions.