AAS  >> Vol. 1 No. 2 (April 2013)

    Vela Jr.:超新星喷发团块与超新星遗骸的互动
    Vela Jr.: Ejecta-Clump Interaction in the Vela Supernova Remnant

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星际介质(RX J0852-4622 Vela Jr.)超新星遗骸(Vela Jr. Vela SNR SN1572)流体力学不稳定性冲击波ISM (RX J0852.0-4622 Vela Jr.); Supernova Remnants (Vela Jr. Vela SNR SN1572); Hydrodynamics; Instabilities; Shock Waves


重迭在船帆座超新星遗骸(Vela supernova remnant)视线上的ROSAT X射线源RX J0852.0-4622,或称Vela Jr.,因其在1.3千电子伏的波段上呈现圆壳外观和检测出44Tiγ射线衰变线所以被认为是新发现的年轻超新星遗骸。然而,观测证据指出Vela Jr.应属于船帆座超新星遗骸的一部份而非独立的物体。二维气体动力学模拟显示,超新星快速的高密度喷发气体物(子弹)可以影响遗骸的外围,产生类似于Vela Jr.的圆环结构。估计Vela Jr.的能量为<0.3 × 1049 erg,相当于1700 km/s<~0.1M的超新星喷发物所注入的动能。我们认为子弹生成最有可能的机制是镍泡效应(nickel bubble effect)。我们预测子弹应该产生辐射,而船帆座超新星遗骸在低X射线亮度的波段上也应存在其它类似的结构。

The ROSAT source RX J0852.0-4622, or Vela Jr., superposed on the Vela supernova remnant, has been identified as a separate young supernova remnant based on its shell-like appearance in X-ray > 1.3 keV and on its detection as a source of the 44Ti γ-ray decay line. However, a re-examination of the observational facts suggests that Vela Jr. should be part of the Vela remnant. We suggest that the shell X-ray feature is produced by a fast ejecta clump (bullet) from the Vela supernova that deposited its kinetic energy in the supernova remnant shell. The estimated energy < 0.3 × 1049 erg could be supplied by a <~0.1M clump moving at1700 km/s. Two-dimensional gas dynamic simulations show that a circular appearance can be produced in the supernova shell under proper conditions. We suggest that the nickel bubble effect is responsible for producing such heavy ejecta clumps in supernovae. There may be other similar X-ray features at a lower brightness level and there may be emission from heavy element ejecta in the object.

王致悦. Vela Jr.:超新星喷发团块与超新星遗骸的互动[J]. 天文与天体物理, 2013, 1(2): 32-37. http://dx.doi.org/10.12677/AAS.2013.12005


[1] B. Aschenbach. Discovery of a young nearby supernova remnant. Nature, 1998, 396: 141-142.
[2] A. N. Cha, K. R. Sembach and A. C. Danks. The distance to the vela supernova remnant. The Astrophysical Journal, 1999, 515(1): L25.
[3] R. Strom, H. M. Johnston, F. Verbunt and B. Aschenbach. A radio-emitting X-ray “bullet” ejected by the Vela supernova. Nature, 1995, 373: 590.
[4] B. Aschenbach, R. Egger and J. Trümper. Discovery of explosion fragments outside the Vela supernova remnant shock-wave boundary. Nature, 1995, 373: 587-590.
[5] A. F. Iyudin, et al. Emission from 44Ti associated with a previously unknown Galactic supernova. Nature, 1998, 396: 142- 144.
[6] B. Aschenbach, A. F. Iyudin and V. Schonelder. Constraints of age, distance and progenitor of the supernova remnant RX J0852.0-4622/GRO J0852-4642. Astronomy and Astrophysics, 1999, 350: 997-1006.
[7] C. P. Burgess, K. Zuber. Footprints of the newly discovered Vela supernova in Antarctic ice cores? Astroparticle Physics, 2000, 14(1): 1.
[8] J. A. Combi, G. E. Romero and P. Benaglia. Radio detection of the supernova remnant RX J0852.0-4622. The Astrophysical Journal, 1999, 519(2): L177.
[9] G. E. Allen, C. B. Markwardt and R. Petre. The high-energy RXTE X-ray spectrum of the recently-discovered remnent RX J0852-4622. Bulletin of the American Astronomical Society. 1999, 31: 862.
[10] P. Slane, J. P. Hughes, R. J. Edgar, P. P. Plucinsky, E. Miyata, H. Tsunemi and B. Aschenbach. RX J0852.0-4622: Another nonther- mal shell-type supernova remnant (G266.2-1.2). The Astrophy- sical Journal, 2001, 548(2): 814.
[11] V. Schonfelder, et al. 44Ti gamma-ray line emission from Cas A and RXJ0852-4622/GROJ0852-4642. In: M. L. McConnell, J. M. Ryan, Eds., AIP Conference Proceedings 510, 5th Compton Symposium, AIP, Melville, 2000: 54-59.
[12] R. Petre, U. Hwang and E. Allen. Evidence for cosmic-ray acceleration in supernova remnants from X-ray observations. Advances in Space Research, 2001, 27(4): 647-652.
[13] H. Tsunemi, E. Miyata and B. Aschenbach. Spectroscopic study of the Vela-shrapnel. Publications of the Astronomical Society of Japan, 1999, 51(5): 711-717.
[14] P. Slane, J. P. Hughes, R. J. Edgar, P. P. Plucinsky, E. Miyata, H. Tsunemi and B. Aschenbach. RX J0852.0-4622: Another nonther- mal shell-type supernova remnant (G266.2-1.2). The Astro- physical Journal, 2001, 548(2): 814.
[15] J. S. Warren, J. P. Hughes and P. O. Slane. Revealing new physical structures in the supernova remnant N63A through chandra imaging spectroscopy. The Astrophysical Journal, 2003, 583(1): 260.
[16] C.-Y. Wang, R. A. Chevalier. Instabilities and clumping in type Ia supernova remnants. The Astrophysical Journal, 2001, 549(2): 1119.
[17] C.-Y. Wang, R. A. Chevalier. Bullets in a core-collapse super- nova remnant: The vela remnant. The Astrophysical Journal, 2002, 574(1): 155.
[18] J. M. Stone, M. L. Norman. ZEUS-2D: A radiation magnetohy- drodynamics code for astrophysical flows in two space dimen- sions. I-The hydrodynamic algorithms and tests. Astrophysical Journal Supplement Series, 1992, 80(2): 753-790.
[19] V. V. Dwarkadas, R. A. Chevalier. Interaction of type Ia super- novae with their surroundings. The Astrophysical Journal, 1998, 497(2): 807.
[20] R. I. Klein, C. F. McKee and P. Colella. On the hydrodynamic interaction of shock waves with interstellar clouds. 1: Nonradia- tive shocks in small clouds. The Astrophysical Journal, 1994, 420(1): 213-216.
[21] U. Hwang, E. V. Gotthelf. X-Ray emission-line imaging and spectroscopy of tycho’s supernova remnant. The Astrophysical Journal, 1997, 475(2): 665.
[22] A. R. Duncan, D. A. Green. The supernova remnant RX J0852.0- 4622: Radio characteristics and implications for SNR statistics. Astronomy and Astrophysics, 2000, 364: 732-740.
[23] F. Bocchino, A. Maggio and S. Sciortino. ROSAT PSPC obser- vation of the NE region of the Vela supernova remnant III. The two-component nature of the X-ray emission and its implications on the ISM. Astronomy and Astrophysics, 1999, 342(3): 839-853.
[24] W. Chen, N. Gehrels. The progenitor of the new COMPTEL/ ROSAT supernova remnant in vela. The Astrophysical Journal, 1999, 514(2): L103.
[25] Cohen, G. Sheldon, Dunn and M. Louise. The lymphocytologists; abell and schenck on anaphylaxis. Allergy and Asthma Proceed- ings, 1991, 12(3): 199-205.
[26] J. M. Blondin, K. J. Borkowski and S. P. Reynolds. Dynamics of Fe bubbles in young su-pernova remnants. The Astrophysical Journal, 2001, 557(2): 782.
[27] H. Li, R. McCray and R. A. Sunyaev. Iron, cobalt, and nickel in SN 1987A. The Astrophysical Journal, 1993, 419: 824.
[28] H. Tsunemi, E. Miyata, B. schenbach, J. Hiraga and D. Akutsu. Over-abundance of calcium in the young SNR RX J0852-4622: evidence of over-production of 44Ti. Publications of the Astro- nomical Society of Japan, 2000, 52: 887-893.
[29] C.-Y. Wang. Clump development by the nickel bubble effect in supernovae. The Astrophysical Journal, 2005, 626(1): 183.
[30] C.-Y. Wang. Nickel Bubble expansion in type Ia supernovae: Adiabatic solutions. The Astrophysical Journal, 2008, 686(1): 337.
[31] C.-Y. Wang. Rayleigh–Taylor instabilities in Type Ia supernova remnants undergoing cosmic ray particle acceleration-low adia- batic index solutions. Monthly Notices of the Royal Astronomi- cal Society, 2011, 415(1): 83-92.
[32] S. Mereghetti. The X-ray sources at the center of the supernova remnant RX J0852.0-4622. The Astrophysical Journal, 2001, 548(2): L213.
[33] G. G. Pavlov, D. Sanwal, B. Kiziltan and G. P. Garmire. The compact central object in the RX J0852.0-4622 supernova remnant. The Astrophysical Journal, 2001, 559(2): L131.
[34] A. F. Iyudin, et al. XMM-Newton observations of the supernova remnant RX J0852.0-4622/GRO J0852-4642. Astron-omy and Astrophysics, 2005, 429(1): 225-234.