A nova remnant is made up of the material either left behind by a sudden explosive fusion eruption by classical novae, or from multiple ejections by recurrent novae. Over their short lifetimes, nova shells show expansion velocities of around 1000 km/s,[1] whose faint nebulosities are usually illuminated by their progenitor stars via light echos as observed with the spherical shell[1] of Nova Persei 1901[2] or the energies remaining in the expanding bubbles like T Pyxidis.[3]
Most novae require a close binary system, with a white dwarf and a main sequence, sub-giant, or red giant star, or the merging of two red dwarfs, so probably all nova remnants must be associated with binaries.[4] This theoretically means these nebula shapes might be affected by their central progenitor stars and the amount of matter ejected by novae.[1] The shapes of these nova nebulae are of much interest to modern astrophysicists.[1][4]
Nova remnants when compared to supernova remnants or planetary nebulae generate much less both in energy and mass. They can be observed for perhaps a few centuries.[1] Notably, more nova remnants have been found with the new novae, due to improved imaging technology like CCD and at other wavelengths. Examples of novae displaying nebula shells or remnants include the following:[1]
^ abcdefLloyd, H.M.; O'Brien, T.J.; Bode, M.F. (1997). "Shaping of nova remnants by binary motion" (PDF). Monthly Notices of the Royal Astronomical Society. 284 (1): 137–147. Bibcode:1997MNRAS.284..137L. doi:10.1093/mnras/284.1.137.
^Liimets, T.; Corradi, R.L.M.; Santander-García, M.; Villaver, E.; Rodríguez-Gil, P.; Verro, K.; Kolka, I. (2014). A dynamical study of the nova remnant of GK Persei / stella novae: Past and future decades. Stellar Novae: Past and Future Decades. ASP Conference Series. Vol. 490. pp. 109–115. arXiv:1310.4488. Bibcode:2014ASPC..490..109L.
^Ogley, R. N.; Chaty, S.; Crocker, M.; Eyres, S. P. S.; Kenworthy, M. A.; Richards, A. M. S.; Rodriguez, L. F.; Stirling, A. M. (April 2002). "A search for radio emission from Galactic supersoft X-ray sources". Monthly Notices of the Royal Astronomical Society. 330 (4): 772–777. arXiv:astro-ph/0111120. Bibcode:2002MNRAS.330..772O. doi:10.1046/j.1365-8711.2002.05130.x. S2CID 3047485. Archived from the original on 5 January 2013.
^ abBode, M.F. (2002). The Evolution of Nova Remnants. International Conference on Classical Nova Explosions. AIP Conference Proceedings. Vol. 637. pp. 497–508. arXiv:astro-ph/0211437. Bibcode:2002AIPC..637..497B. doi:10.1063/1.1518252.
External linksedit
"T Pyxidis". Hubble Site. Nova Remnant. 1997.
. The Carnegie Observatories. Archived from the original on 8 August 2008.
. U. Ottawa. Archived from the original on 5 July 2006.
. U. Ottawa. Archived from the original on 5 July 2006.
April 06, 2024
nova, remnant, nova, remnant, made, material, either, left, behind, sudden, explosive, fusion, eruption, classical, novae, from, multiple, ejections, recurrent, novae, over, their, short, lifetimes, nova, shells, show, expansion, velocities, around, 1000, whos. A nova remnant is made up of the material either left behind by a sudden explosive fusion eruption by classical novae or from multiple ejections by recurrent novae Over their short lifetimes nova shells show expansion velocities of around 1000 km s 1 whose faint nebulosities are usually illuminated by their progenitor stars via light echos as observed with the spherical shell 1 of Nova Persei 1901 2 or the energies remaining in the expanding bubbles like T Pyxidis 3 GK Persei Nova of 1901 remnant Contents 1 Form 2 See also 3 References 4 External linksForm edit nbsp Nova T Pyxidis remnantMost novae require a close binary system with a white dwarf and a main sequence sub giant or red giant star or the merging of two red dwarfs so probably all nova remnants must be associated with binaries 4 This theoretically means these nebula shapes might be affected by their central progenitor stars and the amount of matter ejected by novae 1 The shapes of these nova nebulae are of much interest to modern astrophysicists 1 4 Nova remnants when compared to supernova remnants or planetary nebulae generate much less both in energy and mass They can be observed for perhaps a few centuries 1 Notably more nova remnants have been found with the new novae due to improved imaging technology like CCD and at other wavelengths Examples of novae displaying nebula shells or remnants include the following 1 GK Per RR Pic DQ Her FH Ser V476 Cyg V1974 Cyg HR Del V1500 CygSee also editPlanetary nebula Supernova remnantReferences edit a b c d e f Lloyd H M O Brien T J Bode M F 1997 Shaping of nova remnants by binary motion PDF Monthly Notices of the Royal Astronomical Society 284 1 137 147 Bibcode 1997MNRAS 284 137L doi 10 1093 mnras 284 1 137 Liimets T Corradi R L M Santander Garcia M Villaver E Rodriguez Gil P Verro K Kolka I 2014 A dynamical study of the nova remnant of GK Persei stella novae Past and future decades Stellar Novae Past and Future Decades ASP Conference Series Vol 490 pp 109 115 arXiv 1310 4488 Bibcode 2014ASPC 490 109L Ogley R N Chaty S Crocker M Eyres S P S Kenworthy M A Richards A M S Rodriguez L F Stirling A M April 2002 A search for radio emission from Galactic supersoft X ray sources Monthly Notices of the Royal Astronomical Society 330 4 772 777 arXiv astro ph 0111120 Bibcode 2002MNRAS 330 772O doi 10 1046 j 1365 8711 2002 05130 x S2CID 3047485 Archived from the original on 5 January 2013 a b Bode M F 2002 The Evolution of Nova Remnants International Conference on Classical Nova Explosions AIP Conference Proceedings Vol 637 pp 497 508 arXiv astro ph 0211437 Bibcode 2002AIPC 637 497B doi 10 1063 1 1518252 External links edit T Pyxidis Hubble Site Nova Remnant 1997 Double star systems cycle between big and small blasts The Carnegie Observatories Archived from the original on 8 August 2008 Nova Remnant comparison table U Ottawa Archived from the original on 5 July 2006 Nova Remnant U Ottawa Archived from the original on 5 July 2006 Retrieved from https en wikipedia org w index php title Nova remnant amp oldid 1174810384, wikipedia, wiki, book, books, library,
