Star Formation Regions and Planetary Nebulae
... has been thought that the interaction of the fast wind with AGB ejecta leads to the shaping of the resulting PN. In particular, the presence of a (small) initial asphericity will become amplified, and the variety of PN shapes (spherical, elliptical, butterfly, bipolar, etc.) and structural features ...
... has been thought that the interaction of the fast wind with AGB ejecta leads to the shaping of the resulting PN. In particular, the presence of a (small) initial asphericity will become amplified, and the variety of PN shapes (spherical, elliptical, butterfly, bipolar, etc.) and structural features ...
Chapter 4 Vocabulary
... the process in which particles of an element collide and combine to form a heavier element ...
... the process in which particles of an element collide and combine to form a heavier element ...
Organic compounds: from stars to the solar system
... The delivery of organic compounds from stars to the solar system and its possible implications for the origin of life Ever since the Miller-Urey experiment in 1953, most scientists have held the view that life arose on the early Earth from simple inorganic molecules. With a suitable energy source (e ...
... The delivery of organic compounds from stars to the solar system and its possible implications for the origin of life Ever since the Miller-Urey experiment in 1953, most scientists have held the view that life arose on the early Earth from simple inorganic molecules. With a suitable energy source (e ...
A-105 Homework 1
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
doc - IAC
... We know that, towards the end of their lives, solar-type stars puff off their outer layers, which gradually extend and dilute, eventually blending with the interstellar medium while the stellar remnant follows its evolutionary path until converting itself into a white dwarf – a “star corpse”. Such i ...
... We know that, towards the end of their lives, solar-type stars puff off their outer layers, which gradually extend and dilute, eventually blending with the interstellar medium while the stellar remnant follows its evolutionary path until converting itself into a white dwarf – a “star corpse”. Such i ...
Answer Key 2
... 1. There is an inverse relationship between the mass of a star and the length of its life. True/False lines 1-2 The most massive stars live short lives. 2. The cloud of gas which is created in the supernova explosion a. gradually decreases in size. b. remains luminous for a thousand years. c. is a p ...
... 1. There is an inverse relationship between the mass of a star and the length of its life. True/False lines 1-2 The most massive stars live short lives. 2. The cloud of gas which is created in the supernova explosion a. gradually decreases in size. b. remains luminous for a thousand years. c. is a p ...
Animated Planets PowerPoint Presentation
... Professor Lutz is exploring the physical characteristics of planetary nebulae, their central stars and how planetary nebulae fit into the patterns of stellar evolution. She also analyzes the spectra of symbiotic stars (binaries containing an evolved hot star and a cool star) to determine their chem ...
... Professor Lutz is exploring the physical characteristics of planetary nebulae, their central stars and how planetary nebulae fit into the patterns of stellar evolution. She also analyzes the spectra of symbiotic stars (binaries containing an evolved hot star and a cool star) to determine their chem ...
Mystic nebula
... • Made of light and gases • 21 light years wide on average • Irregular shapes of gas and light • -272 degrees Celsius • Only one degrees above zero ...
... • Made of light and gases • 21 light years wide on average • Irregular shapes of gas and light • -272 degrees Celsius • Only one degrees above zero ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which 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.