In fact, some planetary nebulae emit most of their energy from their solid-state component in the form of far infrared radiation. [50] In January 2005, astronomers announced the first detection of magnetic fields around the central stars of two planetary nebulae, and hypothesized that the fields might be partly or wholly responsible for their remarkable shapes. However, when Huggins looked at the Cat's Eye Nebula, he found a very different spectrum.

Also, partly because of their small total mass, open clusters have relatively poor gravitational cohesion and tend to disperse after a relatively short time, typically from 100 to 600 million years. nebula's central region corresponds to [6] They are a relatively short-lived phenomenon, lasting perhaps a few tens of thousands of years, compared to considerably longer phases of stellar evolution. Planetary Nebula is a misleading name. But Abell 78 shines by the characteristic emission of Planetary nebulae as a phase of stellar evolution Although the existence of planetary nebulae has been known for over 200 years, their origin was not understood until relatively recently.

surface temperatures, The central star is the remnant of its AGB progenitor, an electron-degenerate carbon-oxygen core that has lost most of its hydrogen envelope due to mass loss on the AGB.

The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Current thinking is that the bipolar lobes are created by a high-speed, collimated stellar wind, although the physical origin of the directional nature of this wind is not understood. ", The observations revealed many different shapes, further connecting stellar wind formation to that of planetary nebulae. Spectroscopic observations thus showed that nebulae were made of extremely rarefied gas. Stellar Evolution. doubly ionized oxygen atoms, The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Not. [2] Absorbed ultraviolet light then energizes the shell of nebulous gas around the central star, causing it to appear as a brightly coloured planetary nebula. First the ultraviolet light removes electrons from the atom (in a process called photoionization). The process of making the planetary nebula takes a few thousand years, a blink of the astronomical eye, and the nebula itself only lasts some 20,000 years more before it disperses into interstellar space. The mechanisms that produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role. "Just like a spoon that you stir in a cup of coffee with some milk can create a spiral pattern, the companion sucks material towards it as it revolves around the star and shapes the stellar wind,” said Decin. [14], Herschel assigned these to Class IV of his catalogue of "nebulae", eventually listing 78 "planetary nebulae", most of which are in fact galaxies. The temperature of the gas in the nebula is about 10,000 degrees Celsius, and the central stars of planetary nebulae are among the hottest stars in the Universe, with temperature in the range of 25,000 to over 200,000 degrees Celsius. For the more massive asymptotic giant branch stars that form planetary nebulae, whose progenitors exceed about 3M⊙, their cores will continue to contract.

that our own Sun will experience ... in about 5 billion years. A knowledge of the formation rate of planetary nebulae is crucial to our understanding of a wide range of physical environments and processes, and as such has been fitfully investigated over the last forty or so years. I've read about it for years, but never saw the connection between its location on the Hertsprung-Russell diagram and an asymptote. both cooler (yellowish) and hotter (bluish) than the Sun.

Our current understanding is that stars born with masses in the range of 1 to 8 times the mass of the Sun will evolve through the planetary nebulae stage. He found that many nebulous objects such as the Andromeda Nebula (as it was then known) had spectra that were quite similar. In stellar evolution terms, stars undergoing such increases in luminosity are known as asymptotic giant branch stars (AGB). [17] Electron transitions from these levels in nitrogen and oxygen ions (O+, O2+ (a.k.a. Yet they’re running out of fuel, reduced to fusing carbon in their cores. Planetary nebulae are usually identified by their emission-line spectrum.

By observing such long wavelengths, ALMA penetrates the gas and dust around these stars to reveal details in their winds — and overturning previous assumptions about their shapes. Astrophys. Excellent report. In any case, it's approved now. I read the original article in detail, and I was taken with the quote : "Our results support the claim that binarity may be a prerequisite for the formation of observable aspherical PNe. Jerry Bonnell (UMCP) In this way, planetary nebulae greatly enrich the Milky Way and their nebulae with these heavier elements – collectively known by astronomers as metals and specifically referred to by the metallicity parameter Z.[34]. Rather than a strong continuum with absorption lines superimposed, the Cat's Eye Nebula and other similar objects showed a number of emission lines. This is confirmed by a research note from Menzies (1967) and by the next Sandage paper in 1968 (co-authored with Katem & Kristian). Whether these companions are stars or giant planets, they are likely affecting the evolving shapes of the stellar winds. Planetary Nebula 14.9 - Understand the principal stages and timescales of stellar evolution for stars of similar mass to the Sun, including: c) planetary nebula Planetary Nebula is a misleading name.

NASA Web Recent observations by infrared and millimeter-wave telescopes have found that planetary nebulae contain, in addition to atoms, molecules and solid-state particles. The most well known planetary nebula is the Ring Nebula in the constellation of Lyra (Figure 1), which can easily be observed with a small telescope in summer from the Northern hemisphere. featured, along with a brief explanation written by a professional astronomer.

The density in the nebulae is very low, ranging from several hundred to a million atoms per cubic centimeter.

[41], The huge variety of the shapes is partially the projection effect—the same nebula when viewed under different angles will appear different. They are found mostly near the plane of the Milky Way, with the greatest concentration near the galactic center. Planetary nebula Abell 78 Now, a team of observers has looked one step earlier in stellar evolution to explain how these shapes come to be. Headquartered in Cambridge, Mass., the Center for Astrophysics | Harvard & Smithsonian (CfA) is a collaboration between the Smithsonian Astrophysical Observatory and the Harvard College Observatory.

2006). All of them have some form of arcs or shells, and some of them even exhibit the kinds of spiral, bipolar, or eye-like shapes that planetary nebulae have. [9] Brightest of these was at a wavelength of 500.7 nanometres, which did not correspond with a line of any known element. In 1970, Polish astronomer Bohdan Paczynski established that the central stars of planetary nebulae are cores of asymptotic giant branch stars (a type of very old red giants) and that they generate energy by nuclear burning of hydrogen in a shell above the core (Paczynski 1970).

Dust and Gas Protostar Brown Dwarf. The Hubble gallery image reminds me of looking through a microscope at a drop of pond water. Other articles where Planetary-nebula phase is discussed: white dwarf star: This is the planetary-nebula phase. Discover the cosmos!

These fantastic gas-and-dust eruptions from low-mass stars form shapes such as spirals, roses, butterflies, and even cosmic eyes. Decin et al. The nebula is illuminated by a central star, which sometimes is too faint to be seen. When stars formed earlier in the universe they theoretically contained smaller quantities of heavier elements. [53] However, there is currently only one case of a planetary nebula discovered in an open cluster that is agreed upon by independent researchers. Astr. Although many planetary nebulae have shell-like structures similar to that of the Ring Nebula, some show butterfly-like structures with a pair of bipolar lobes (Figure 3). A more extensive description of our modern understanding of the origin and evolution of planetary nebulae can be found in this book. ", About Center for Astrophysics | Harvard & Smithsonian.

All rights reserved. Sky & Telescope is part of AAS Sky Publishing, LLC, a wholly owned subsidiary of the American Astronomical Society. (MTU) & [7] Once all of the red giant's atmosphere has been dissipated, energetic ultraviolet radiation from the exposed hot luminous core, called a planetary nebula nucleus (PNN), ionizes the ejected material.

Most recent discoveries of new planetary nebulae are the result of imaging surveys of the Galaxy using a narrow-band filter around the Hα line of hydrogen (Parker et al.

A similar idea had led to the discovery of helium through analysis of the Sun's spectrum in 1868. [47] Gravitational interactions with companion stars if the central stars are binary stars may be one cause. In the latter case, there are not enough UV photons being emitted by the central star to ionize all the surrounding gas, and an ionization front propagates outward into the circumstellar envelope of neutral atoms. ejection, collimation, and precession. "The lack of such detailed observational data caused us to initially assume that the stellar winds have an overall spherical geometry, much like the stars they surround," said Gottlieb.

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In fact, some planetary nebulae emit most of their energy from their solid-state component in the form of far infrared radiation. [50] In January 2005, astronomers announced the first detection of magnetic fields around the central stars of two planetary nebulae, and hypothesized that the fields might be partly or wholly responsible for their remarkable shapes. However, when Huggins looked at the Cat's Eye Nebula, he found a very different spectrum.

Also, partly because of their small total mass, open clusters have relatively poor gravitational cohesion and tend to disperse after a relatively short time, typically from 100 to 600 million years. nebula's central region corresponds to [6] They are a relatively short-lived phenomenon, lasting perhaps a few tens of thousands of years, compared to considerably longer phases of stellar evolution. Planetary Nebula is a misleading name. But Abell 78 shines by the characteristic emission of Planetary nebulae as a phase of stellar evolution Although the existence of planetary nebulae has been known for over 200 years, their origin was not understood until relatively recently.

surface temperatures, The central star is the remnant of its AGB progenitor, an electron-degenerate carbon-oxygen core that has lost most of its hydrogen envelope due to mass loss on the AGB.

The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Current thinking is that the bipolar lobes are created by a high-speed, collimated stellar wind, although the physical origin of the directional nature of this wind is not understood. ", The observations revealed many different shapes, further connecting stellar wind formation to that of planetary nebulae. Spectroscopic observations thus showed that nebulae were made of extremely rarefied gas. Stellar Evolution. doubly ionized oxygen atoms, The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Not. [2] Absorbed ultraviolet light then energizes the shell of nebulous gas around the central star, causing it to appear as a brightly coloured planetary nebula. First the ultraviolet light removes electrons from the atom (in a process called photoionization). The process of making the planetary nebula takes a few thousand years, a blink of the astronomical eye, and the nebula itself only lasts some 20,000 years more before it disperses into interstellar space. The mechanisms that produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role. "Just like a spoon that you stir in a cup of coffee with some milk can create a spiral pattern, the companion sucks material towards it as it revolves around the star and shapes the stellar wind,” said Decin. [14], Herschel assigned these to Class IV of his catalogue of "nebulae", eventually listing 78 "planetary nebulae", most of which are in fact galaxies. The temperature of the gas in the nebula is about 10,000 degrees Celsius, and the central stars of planetary nebulae are among the hottest stars in the Universe, with temperature in the range of 25,000 to over 200,000 degrees Celsius. For the more massive asymptotic giant branch stars that form planetary nebulae, whose progenitors exceed about 3M⊙, their cores will continue to contract.

that our own Sun will experience ... in about 5 billion years. A knowledge of the formation rate of planetary nebulae is crucial to our understanding of a wide range of physical environments and processes, and as such has been fitfully investigated over the last forty or so years. I've read about it for years, but never saw the connection between its location on the Hertsprung-Russell diagram and an asymptote. both cooler (yellowish) and hotter (bluish) than the Sun.

Our current understanding is that stars born with masses in the range of 1 to 8 times the mass of the Sun will evolve through the planetary nebulae stage. He found that many nebulous objects such as the Andromeda Nebula (as it was then known) had spectra that were quite similar. In stellar evolution terms, stars undergoing such increases in luminosity are known as asymptotic giant branch stars (AGB). [17] Electron transitions from these levels in nitrogen and oxygen ions (O+, O2+ (a.k.a. Yet they’re running out of fuel, reduced to fusing carbon in their cores. Planetary nebulae are usually identified by their emission-line spectrum.

By observing such long wavelengths, ALMA penetrates the gas and dust around these stars to reveal details in their winds — and overturning previous assumptions about their shapes. Astrophys. Excellent report. In any case, it's approved now. I read the original article in detail, and I was taken with the quote : "Our results support the claim that binarity may be a prerequisite for the formation of observable aspherical PNe. Jerry Bonnell (UMCP) In this way, planetary nebulae greatly enrich the Milky Way and their nebulae with these heavier elements – collectively known by astronomers as metals and specifically referred to by the metallicity parameter Z.[34]. Rather than a strong continuum with absorption lines superimposed, the Cat's Eye Nebula and other similar objects showed a number of emission lines. This is confirmed by a research note from Menzies (1967) and by the next Sandage paper in 1968 (co-authored with Katem & Kristian). Whether these companions are stars or giant planets, they are likely affecting the evolving shapes of the stellar winds. Planetary Nebula 14.9 - Understand the principal stages and timescales of stellar evolution for stars of similar mass to the Sun, including: c) planetary nebula Planetary Nebula is a misleading name.

NASA Web Recent observations by infrared and millimeter-wave telescopes have found that planetary nebulae contain, in addition to atoms, molecules and solid-state particles. The most well known planetary nebula is the Ring Nebula in the constellation of Lyra (Figure 1), which can easily be observed with a small telescope in summer from the Northern hemisphere. featured, along with a brief explanation written by a professional astronomer.

The density in the nebulae is very low, ranging from several hundred to a million atoms per cubic centimeter.

[41], The huge variety of the shapes is partially the projection effect—the same nebula when viewed under different angles will appear different. They are found mostly near the plane of the Milky Way, with the greatest concentration near the galactic center. Planetary nebula Abell 78 Now, a team of observers has looked one step earlier in stellar evolution to explain how these shapes come to be. Headquartered in Cambridge, Mass., the Center for Astrophysics | Harvard & Smithsonian (CfA) is a collaboration between the Smithsonian Astrophysical Observatory and the Harvard College Observatory.

2006). All of them have some form of arcs or shells, and some of them even exhibit the kinds of spiral, bipolar, or eye-like shapes that planetary nebulae have. [9] Brightest of these was at a wavelength of 500.7 nanometres, which did not correspond with a line of any known element. In 1970, Polish astronomer Bohdan Paczynski established that the central stars of planetary nebulae are cores of asymptotic giant branch stars (a type of very old red giants) and that they generate energy by nuclear burning of hydrogen in a shell above the core (Paczynski 1970).

Dust and Gas Protostar Brown Dwarf. The Hubble gallery image reminds me of looking through a microscope at a drop of pond water. Other articles where Planetary-nebula phase is discussed: white dwarf star: This is the planetary-nebula phase. Discover the cosmos!

These fantastic gas-and-dust eruptions from low-mass stars form shapes such as spirals, roses, butterflies, and even cosmic eyes. Decin et al. The nebula is illuminated by a central star, which sometimes is too faint to be seen. When stars formed earlier in the universe they theoretically contained smaller quantities of heavier elements. [53] However, there is currently only one case of a planetary nebula discovered in an open cluster that is agreed upon by independent researchers. Astr. Although many planetary nebulae have shell-like structures similar to that of the Ring Nebula, some show butterfly-like structures with a pair of bipolar lobes (Figure 3). A more extensive description of our modern understanding of the origin and evolution of planetary nebulae can be found in this book. ", About Center for Astrophysics | Harvard & Smithsonian.

All rights reserved. Sky & Telescope is part of AAS Sky Publishing, LLC, a wholly owned subsidiary of the American Astronomical Society. (MTU) & [7] Once all of the red giant's atmosphere has been dissipated, energetic ultraviolet radiation from the exposed hot luminous core, called a planetary nebula nucleus (PNN), ionizes the ejected material.

Most recent discoveries of new planetary nebulae are the result of imaging surveys of the Galaxy using a narrow-band filter around the Hα line of hydrogen (Parker et al.

A similar idea had led to the discovery of helium through analysis of the Sun's spectrum in 1868. [47] Gravitational interactions with companion stars if the central stars are binary stars may be one cause. In the latter case, there are not enough UV photons being emitted by the central star to ionize all the surrounding gas, and an ionization front propagates outward into the circumstellar envelope of neutral atoms. ejection, collimation, and precession. "The lack of such detailed observational data caused us to initially assume that the stellar winds have an overall spherical geometry, much like the stars they surround," said Gottlieb.

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stellar evolution planetary nebula

They are extended in size and fuzzy in appearance, and generally show some degree of symmetry. hydrogen atoms.

By: Monica Young [27] This state of equilibrium is known as the main sequence, which can last for tens of millions to billions of years, depending on the mass. Soc., 373, 79, Schönberner, D (1981) Late stages of stellar evolution - Central stars of planetary nebulae, Astr.

The first planetary nebula discovered (though not yet termed as such) was the Dumbbell Nebula in the constellation of Vulpecula. Comparison of the spectra of planetary nebulae at different stages of evolution show that these compounds are synthesized quickly over timescales of the order of hundreds of years (Kwok 2004). ", Morgan MacLeod's quote is slightly overstated IMO. [62], The distances to planetary nebulae are generally poorly determined.

In fact, some planetary nebulae emit most of their energy from their solid-state component in the form of far infrared radiation. [50] In January 2005, astronomers announced the first detection of magnetic fields around the central stars of two planetary nebulae, and hypothesized that the fields might be partly or wholly responsible for their remarkable shapes. However, when Huggins looked at the Cat's Eye Nebula, he found a very different spectrum.

Also, partly because of their small total mass, open clusters have relatively poor gravitational cohesion and tend to disperse after a relatively short time, typically from 100 to 600 million years. nebula's central region corresponds to [6] They are a relatively short-lived phenomenon, lasting perhaps a few tens of thousands of years, compared to considerably longer phases of stellar evolution. Planetary Nebula is a misleading name. But Abell 78 shines by the characteristic emission of Planetary nebulae as a phase of stellar evolution Although the existence of planetary nebulae has been known for over 200 years, their origin was not understood until relatively recently.

surface temperatures, The central star is the remnant of its AGB progenitor, an electron-degenerate carbon-oxygen core that has lost most of its hydrogen envelope due to mass loss on the AGB.

The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Current thinking is that the bipolar lobes are created by a high-speed, collimated stellar wind, although the physical origin of the directional nature of this wind is not understood. ", The observations revealed many different shapes, further connecting stellar wind formation to that of planetary nebulae. Spectroscopic observations thus showed that nebulae were made of extremely rarefied gas. Stellar Evolution. doubly ionized oxygen atoms, The findings, published in Science, contradict common consensus, and show that not only are stellar winds aspherical, but they also share similarities with planetary nebulae. Not. [2] Absorbed ultraviolet light then energizes the shell of nebulous gas around the central star, causing it to appear as a brightly coloured planetary nebula. First the ultraviolet light removes electrons from the atom (in a process called photoionization). The process of making the planetary nebula takes a few thousand years, a blink of the astronomical eye, and the nebula itself only lasts some 20,000 years more before it disperses into interstellar space. The mechanisms that produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role. "Just like a spoon that you stir in a cup of coffee with some milk can create a spiral pattern, the companion sucks material towards it as it revolves around the star and shapes the stellar wind,” said Decin. [14], Herschel assigned these to Class IV of his catalogue of "nebulae", eventually listing 78 "planetary nebulae", most of which are in fact galaxies. The temperature of the gas in the nebula is about 10,000 degrees Celsius, and the central stars of planetary nebulae are among the hottest stars in the Universe, with temperature in the range of 25,000 to over 200,000 degrees Celsius. For the more massive asymptotic giant branch stars that form planetary nebulae, whose progenitors exceed about 3M⊙, their cores will continue to contract.

that our own Sun will experience ... in about 5 billion years. A knowledge of the formation rate of planetary nebulae is crucial to our understanding of a wide range of physical environments and processes, and as such has been fitfully investigated over the last forty or so years. I've read about it for years, but never saw the connection between its location on the Hertsprung-Russell diagram and an asymptote. both cooler (yellowish) and hotter (bluish) than the Sun.

Our current understanding is that stars born with masses in the range of 1 to 8 times the mass of the Sun will evolve through the planetary nebulae stage. He found that many nebulous objects such as the Andromeda Nebula (as it was then known) had spectra that were quite similar. In stellar evolution terms, stars undergoing such increases in luminosity are known as asymptotic giant branch stars (AGB). [17] Electron transitions from these levels in nitrogen and oxygen ions (O+, O2+ (a.k.a. Yet they’re running out of fuel, reduced to fusing carbon in their cores. Planetary nebulae are usually identified by their emission-line spectrum.

By observing such long wavelengths, ALMA penetrates the gas and dust around these stars to reveal details in their winds — and overturning previous assumptions about their shapes. Astrophys. Excellent report. In any case, it's approved now. I read the original article in detail, and I was taken with the quote : "Our results support the claim that binarity may be a prerequisite for the formation of observable aspherical PNe. Jerry Bonnell (UMCP) In this way, planetary nebulae greatly enrich the Milky Way and their nebulae with these heavier elements – collectively known by astronomers as metals and specifically referred to by the metallicity parameter Z.[34]. Rather than a strong continuum with absorption lines superimposed, the Cat's Eye Nebula and other similar objects showed a number of emission lines. This is confirmed by a research note from Menzies (1967) and by the next Sandage paper in 1968 (co-authored with Katem & Kristian). Whether these companions are stars or giant planets, they are likely affecting the evolving shapes of the stellar winds. Planetary Nebula 14.9 - Understand the principal stages and timescales of stellar evolution for stars of similar mass to the Sun, including: c) planetary nebula Planetary Nebula is a misleading name.

NASA Web Recent observations by infrared and millimeter-wave telescopes have found that planetary nebulae contain, in addition to atoms, molecules and solid-state particles. The most well known planetary nebula is the Ring Nebula in the constellation of Lyra (Figure 1), which can easily be observed with a small telescope in summer from the Northern hemisphere. featured, along with a brief explanation written by a professional astronomer.

The density in the nebulae is very low, ranging from several hundred to a million atoms per cubic centimeter.

[41], The huge variety of the shapes is partially the projection effect—the same nebula when viewed under different angles will appear different. They are found mostly near the plane of the Milky Way, with the greatest concentration near the galactic center. Planetary nebula Abell 78 Now, a team of observers has looked one step earlier in stellar evolution to explain how these shapes come to be. Headquartered in Cambridge, Mass., the Center for Astrophysics | Harvard & Smithsonian (CfA) is a collaboration between the Smithsonian Astrophysical Observatory and the Harvard College Observatory.

2006). All of them have some form of arcs or shells, and some of them even exhibit the kinds of spiral, bipolar, or eye-like shapes that planetary nebulae have. [9] Brightest of these was at a wavelength of 500.7 nanometres, which did not correspond with a line of any known element. In 1970, Polish astronomer Bohdan Paczynski established that the central stars of planetary nebulae are cores of asymptotic giant branch stars (a type of very old red giants) and that they generate energy by nuclear burning of hydrogen in a shell above the core (Paczynski 1970).

Dust and Gas Protostar Brown Dwarf. The Hubble gallery image reminds me of looking through a microscope at a drop of pond water. Other articles where Planetary-nebula phase is discussed: white dwarf star: This is the planetary-nebula phase. Discover the cosmos!

These fantastic gas-and-dust eruptions from low-mass stars form shapes such as spirals, roses, butterflies, and even cosmic eyes. Decin et al. The nebula is illuminated by a central star, which sometimes is too faint to be seen. When stars formed earlier in the universe they theoretically contained smaller quantities of heavier elements. [53] However, there is currently only one case of a planetary nebula discovered in an open cluster that is agreed upon by independent researchers. Astr. Although many planetary nebulae have shell-like structures similar to that of the Ring Nebula, some show butterfly-like structures with a pair of bipolar lobes (Figure 3). A more extensive description of our modern understanding of the origin and evolution of planetary nebulae can be found in this book. ", About Center for Astrophysics | Harvard & Smithsonian.

All rights reserved. Sky & Telescope is part of AAS Sky Publishing, LLC, a wholly owned subsidiary of the American Astronomical Society. (MTU) & [7] Once all of the red giant's atmosphere has been dissipated, energetic ultraviolet radiation from the exposed hot luminous core, called a planetary nebula nucleus (PNN), ionizes the ejected material.

Most recent discoveries of new planetary nebulae are the result of imaging surveys of the Galaxy using a narrow-band filter around the Hα line of hydrogen (Parker et al.

A similar idea had led to the discovery of helium through analysis of the Sun's spectrum in 1868. [47] Gravitational interactions with companion stars if the central stars are binary stars may be one cause. In the latter case, there are not enough UV photons being emitted by the central star to ionize all the surrounding gas, and an ionization front propagates outward into the circumstellar envelope of neutral atoms. ejection, collimation, and precession. "The lack of such detailed observational data caused us to initially assume that the stellar winds have an overall spherical geometry, much like the stars they surround," said Gottlieb.

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