Scioly Astro DSOS 22/23
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Last updated 4:56 AM on 3/11/23
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16 Terms
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AG Carinae
* luminous blue variable
* in transition phase between massive class O blue supergiant and a Wolf-Rayet star
* Highly unstable, suffers from erratic pulsations
* in transition phase between massive class O blue supergiant and a Wolf-Rayet star
* Highly unstable, suffers from erratic pulsations
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GW170817
* Gravitational wave originating from shell elliptical galaxy NGC 4993
* Produced by the last minutes of a two binary neutron stars' inspiral process, ending with a merger.
* Produced by the last minutes of a two binary neutron stars' inspiral process, ending with a merger.
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PSR J2030+4415
* Pulsar which has generated a beam of matter and antimatter (a filament) 40 trillion miles long
* Could help explain presence of positrons detected throughout Milky Way galaxy and on Earth
* 3 rpm
* bow shock moves in front of pulsar
* Could help explain presence of positrons detected throughout Milky Way galaxy and on Earth
* 3 rpm
* bow shock moves in front of pulsar
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R Hydrae
* Mira type variable: aging red giant with a stellar classification of M6e/M9e, currently near the thermal-pulsing tip of the asymptotic giant branch.
* has a detached, expanding shell of dust around it
* well known for declining period. In the past few decades, the period of R Hya has declined by over a hundred days.
* has a bow shock, first mira type var to be seen with bow shock
* has a detached, expanding shell of dust around it
* well known for declining period. In the past few decades, the period of R Hya has declined by over a hundred days.
* has a bow shock, first mira type var to be seen with bow shock
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R Aquarii
* symbiotic star believed to contain a white dwarf and a Mira-type variable in a binary system
* The main Mira-type star is a red giant, and varies in brightness by a factor of several hundred and with a period of slightly more than a year. The two components have been resolved at a separation of 55 mas.
* orbital period 44 years
* The main Mira-type star is a red giant, and varies in brightness by a factor of several hundred and with a period of slightly more than a year. The two components have been resolved at a separation of 55 mas.
* orbital period 44 years
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NGC 7027
* Jewel Bug Nebula, planetary nebula 3000 LY from Earth -One of the smallest planetary nebulae and by far the most extensively studied
* It is 600 years old and measures only 0.2 by 0.1 light years
* NGC 7027 has a rich and highly ionized spectrum caused by its hot central star.
* NGC 7027's central star was identified in a new wavelength of light — near-ultraviolet
* It is 600 years old and measures only 0.2 by 0.1 light years
* NGC 7027 has a rich and highly ionized spectrum caused by its hot central star.
* NGC 7027's central star was identified in a new wavelength of light — near-ultraviolet
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RS Puppis
* long-period Cepheid variable star 6000 LY away
* one of the biggest and brightest known Cepheids in the Milky Way galaxy and has one of the longest periods for this class of star at 41.5 days.
* standard candle
* supergiant with a spectral classification of G2Ib
* one of the biggest and brightest known Cepheids in the Milky Way galaxy and has one of the longest periods for this class of star at 41.5 days.
* standard candle
* supergiant with a spectral classification of G2Ib
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NaSt1
* Wolf-Rayet star
* Normal Wolf-Rayet stars eject fast-flying gas out of their poles, but NaSt1 had a pancake-shaped disk of gas instead, hinting at mass transfer to a binary companion
* Hard to measure anything between Nasty and companion due to the heavy dust
* Normal Wolf-Rayet stars eject fast-flying gas out of their poles, but NaSt1 had a pancake-shaped disk of gas instead, hinting at mass transfer to a binary companion
* Hard to measure anything between Nasty and companion due to the heavy dust
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HD 184738
* WC star at the center of a small planetary nebula. The main difference between WC and Wolf-Rayet stars are that Wolf-Rayet stars are rich in Nitrogen with some Carbon in their atmospheres while WC stars are rich in Carbon and Oxygen with little or no Nitrogen.
* Very bright in infrared spectrum
* Very bright in infrared spectrum
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W Virginis
* Prototype W Virginis variable--subclass of Cepheid variable
* Spectral type: F0Ib-G0Ib
* variations in the light curve apparently due to multiple pulsation periods rather than inherent instabilities in the pulsation.
* W Virginis stars are old helium shell burning stars with masses less than the sun. They have supergiant spectral luminosity classes despite their modest masses and actual luminosities, because they are highly inflated evolved stars with very low surface gravities
* Spectral type: F0Ib-G0Ib
* variations in the light curve apparently due to multiple pulsation periods rather than inherent instabilities in the pulsation.
* W Virginis stars are old helium shell burning stars with masses less than the sun. They have supergiant spectral luminosity classes despite their modest masses and actual luminosities, because they are highly inflated evolved stars with very low surface gravities
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G344.7-0.1
* Type Ia supernova remnant
* 3,000 to 6,000 years old
* gives astronomers a window into an important phase later in the evolution of a Type Ia supernova remnant
* Expanding blast wave and the stellar debris produce X-rays in supernova remnants. As the debris moves outward from the initial explosion, it encounters resistance from surrounding gas and slows down, creating a reverse shock wave that travels back toward the center of the explosion. The reverse shock heats the debris to millions of degrees, causing it to glow in X-rays.
* 3,000 to 6,000 years old
* gives astronomers a window into an important phase later in the evolution of a Type Ia supernova remnant
* Expanding blast wave and the stellar debris produce X-rays in supernova remnants. As the debris moves outward from the initial explosion, it encounters resistance from surrounding gas and slows down, creating a reverse shock wave that travels back toward the center of the explosion. The reverse shock heats the debris to millions of degrees, causing it to glow in X-rays.
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SS Cygni
* cataclysmic variable star prototype of dwarf novae, which are comprised of a close binary system with a white dwarf primary star and a red dwarf secondary star
* One of the components is a red dwarf-type star, cooler than the Sun, while the other is a white dwarf, separated only by 100,000 miles or less
* the main sequence star loses matter which is streamed in the direction of the primary, forming an accretion disk around the white dwarf star.
* SS Cyg's light curve reveals ever-changing intervals of wide and narrow outbursts, of about 18 and 8-day durations, respectively
* One of the components is a red dwarf-type star, cooler than the Sun, while the other is a white dwarf, separated only by 100,000 miles or less
* the main sequence star loses matter which is streamed in the direction of the primary, forming an accretion disk around the white dwarf star.
* SS Cyg's light curve reveals ever-changing intervals of wide and narrow outbursts, of about 18 and 8-day durations, respectively
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E0102-72.3
* Neutron star located in supernova remnant E0102 in the Small Magellanic cloud
* Oxygen-rich supernova remnants like E0102 are important for understanding how massive stars fuse lighter elements into heavier ones before they explode.
* The neutron star is an isolated neutron star created in the supernova explosion about two millennia ago. The lack of evidence for extended radio emission or pulsed X-ray radiation, typically associated with rapidly rotating highly-magnetized neutron stars, indicates that the astronomers have detected the X-radiation from the hot surface of an isolated neutron star with low magnetic fields. About ten such objects have been detected in the Milky Way galaxy, but this is the first one detected outside our galaxy.
* The neutron star is offset from the center of the circular shell of X-ray emission produced by the blast wave of the supernova
* Oxygen-rich supernova remnants like E0102 are important for understanding how massive stars fuse lighter elements into heavier ones before they explode.
* The neutron star is an isolated neutron star created in the supernova explosion about two millennia ago. The lack of evidence for extended radio emission or pulsed X-ray radiation, typically associated with rapidly rotating highly-magnetized neutron stars, indicates that the astronomers have detected the X-radiation from the hot surface of an isolated neutron star with low magnetic fields. About ten such objects have been detected in the Milky Way galaxy, but this is the first one detected outside our galaxy.
* The neutron star is offset from the center of the circular shell of X-ray emission produced by the blast wave of the supernova
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47 Tucanae
* Globular cluster
* 47 Tucanae has 25 known millisecond pulsars, the second largest population of pulsars in any globular cluster.
* Could have a possible central black hole, but its existence is disputed
* 47 Tucanae has 25 known millisecond pulsars, the second largest population of pulsars in any globular cluster.
* Could have a possible central black hole, but its existence is disputed
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X9
\
* White dwarf orbiting a black hole at 2.5 times distance between Earth and moon at 12 million km/hr. -25 minute period
* Before ATCA data in 2015, astronomers thought it was a cataclysmic variable
* the white dwarf is so close to the black hole that much of its material is being pulled away. If it continues to lose mass, this white dwarf may evolve into some exotic sort of planet or completely evaporate.
* White dwarf orbiting a black hole at 2.5 times distance between Earth and moon at 12 million km/hr. -25 minute period
* Before ATCA data in 2015, astronomers thought it was a cataclysmic variable
* the white dwarf is so close to the black hole that much of its material is being pulled away. If it continues to lose mass, this white dwarf may evolve into some exotic sort of planet or completely evaporate.
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SN 2008D
* Type Ibc Supernova
* The explosion of the supernova precursor star was in the spiral galaxy NGC 2770
* first time that astronomers have ever observed a supernova as it occurred.
* 2008D exploded with an energy that put it between a supernova and a hypernova.
* The explosion was off-center, with gas on one side of the explosion moving outward faster than on the other.
* The explosion of the supernova precursor star was in the spiral galaxy NGC 2770
* first time that astronomers have ever observed a supernova as it occurred.
* 2008D exploded with an energy that put it between a supernova and a hypernova.
* The explosion was off-center, with gas on one side of the explosion moving outward faster than on the other.