Ia型超新星爆炸由於其標準燭光特性，在宇宙學研究上具有重要地位。
基於單一簡併模型(single-degenerate scenario)，近期的理論與數值研究認
為在此模型中的非簡併態伴星可以在爆炸中存活，且爆炸對其造成的影響
能使伴星在爆炸後更亮。然而，觀測上並沒有在銀河系附近的超新星殘骸
中看到足夠多存活下來的伴星。在這個研究中，我們藉由爆炸的二維流體
力學模擬與長時間的恆星演化模擬去研究超新星爆炸對伴星的影響。我們
考慮了更多樣的富含氫氣的伴星，並系統性的分析爆炸對其伴星的影響。
這個工作可以解釋為什麼在鄰近的超新星爆炸殘骸中，我們沒有觀測到許
多存活下來的伴星。
這篇論文的架構如下:第一章會是Ia型超新星的介紹；第二章是我們對這
些伴星所作的研究；最後一章則是這邊論文的總結。

Type Ia supernovae are important as standardizable candles for cosmo-
logical research. Within the single-degenerate scenario, recent theoretical
and numerical studies of Type Ia supernova explosions suggest that non-
degenerate companions could survive and the supernova impact could let
the companion star be luminous after the explosion. However, the surviv-
ing ex-companions are still not firmly detected in observations of nearby
type Ia supernova remnants. In this project, we investigate the response
of surviving companions via two-dimensional hydrodynamics simulations of
supernova ejecta on binary companions and the subsequent long-term stel-
lar evolution of surviving companions. We consider a wide range of possible
hydrogen-rich companions and characterize the companion response system-
atically. This work can explain the non-detection of surviving companions
in nearby supernova remnants.
This thesis consists of three sections. The first chapter is a brief intro-
duction of type Ia supernovae. The second chapter is the work we have
done on the investigation of supernova impact and evolution of surviving
companions. The last chapter will be the summary.

[1] Bauer, E. B., White, C. J., & Bildsten, L. 2019, ApJ, 887, 68
[2] Bedin, L. R., Ruiz-Lapuente, P., González Hernández, J. I., et al. 2014, MN-
RAS, 439, 354
[3] Branch,
D.
&
Tammann,
G.
A.
1992,
ARA&A,
30,
359.
doi:10.1146/annurev.aa.30.090192.002043
[4] Couch, S. M., Graziani, C., & Flocke, N. 2013, ApJ, 778, 181.
doi:10.1088/0004-637X/778/2/181
[5] Di Stefano, R., Voss, R., & Claeys, J. S. W. 2011, ApJL, 738, L1
[6] Dubey, A., Reid, L. B., & Fisher, R. 2008, Physica Scripta Volume T, 132,
014046
[7] Eggleton, P. P. 1983, ApJ, 268, 368
[8] Fryxell, B., Olson, K., Ricker, P., et al. 2000, ApJS, 131, 273
[9] Goldhaber, G., Groom, D. E., Kim, A., et al. 2001, ApJ, 558, 359.
doi:10.1086/322460
[10] González Hernández, J. I., Ruiz-Lapuente, P., Tabernero, H. M., et al. 2012,
Nature, 489, 533. doi:10.1038/nature11447
[11] González Hernández, J. I., Ruiz-Lapuente, P., Filippenko, A. V., et al. 2009,
ApJ, 691, 1. doi:10.1088/0004-637X/691/1/1
[12] Hillebrandt, W., Kromer, M., Röpke, F. K., et al. 2013, Frontiers of Physics,
8, 116. doi:10.1007/s11467-013-0303-2
[13] González Hernández, J. I., Ruiz-Lapuente, P., Filippenko, A. V., et al. 2009,
ApJ, 691, 1
[14] Kerzendorf, W. E., Strampelli, G., Shen, K. J., et al. 2018, MNRAS, 479,
192. doi:10.1093/mnras/sty1357
[15] Kerzendorf, W. E., Yong, D., Schmidt, B. P., et al. 2013, ApJ, 774, 99.
doi:10.1088/0004-637X/774/2/99
[16] Knop, R. A., Aldering, G., Amanullah, R., et al. 2003, ApJ, 598, 102.
doi:10.1086/378560
[17] Li, C.-J., Kerzendorf, W. E., Chu, Y.-H., et al. 2019, ApJ, 886, 99
[18] Li, C.-J., Chu, Y.-H., Gruendl, R. A., et al. 2017, ApJ, 836, 85.
doi:10.3847/1538-4357/836/1/85
[19] Litke, K. C., Chu, Y.-H., Holmes, A., et al. 2017, ApJ, 837, 111.
doi:10.3847/1538-4357/aa5d57
[20] Liu, Z.-W., Pakmor, R., Röpke, F. K., et al. 2013, A&A, 554, A109.
doi:10.1051/0004-6361/201220903
[21] Nomoto, K., Thielemann, F.-K., & Yokoi, K. 1984, ApJ, 286, 644
[22] Nomoto, K. 1982, ApJ, 257, 780. doi:10.1086/160031
[23] Pagnotta, A. & Schaefer, B. E. 2015, ApJ, 799, 101. doi:10.1088/0004-
637X/799/1/101
[24] Pakmor, R., Röpke, F. K., Weiss, A., et al. 2008, A&A, 489, 943.
doi:10.1051/0004-6361:200810456
[25] Pan, K.-C., Ricker, P. M., & Taam, R. E. 2010, ApJ, 715, 78.
doi:10.1088/0004-637X/715/1/78
[26] Pan, K.-C., Ricker, P. M., & Taam, R. E. 2010, ApJ, 715, 78.
doi:10.1088/0004-637X/715/1/78
[27] Pan, K.-C., Ricker, P. M., & Taam, R. E. 2012, ApJ, 750, 151.
doi:10.1088/0004-637X/750/2/151
[28] Pan, K.-C., Ricker, P. M., & Taam, R. E. 2012, ApJ, 760, 21.
doi:10.1088/0004-637X/760/1/21
[29] Paxton, B., Bildsten, L., Dotter, A., et al. 2011, ApJS, 192, 3
[30] Paxton, B., Cantiello, M., Arras, P., et al. 2013, ApJS, 208, 4
[31] Paxton, B., Marchant, P., Schwab, J., et al. 2015, ApJS, 220, 15
[32] Paxton, B., Schwab, J., Bauer, E. B., et al. 2018, ApJS, 234, 34
[33] Paxton, B., Smolec, R., Schwab, J., et al. 2019, ApJS, 243, 10
[34] Perlmutter, S., Aldering, G., Goldhaber, G., et al. 1999, ApJ, 517, 565.
[35] Phillips, M. M. 1993, ApJL, 413, L105. doi:10.1086/186970
[36] Riess, A. G., Filippenko, A. V., Challis, P., et al. 1998, AJ, 116, 1009
[37] Ruiz-Lapuente, P., Damiani, F., Bedin, L., et al. 2018, ApJ, 862, 124.
doi:10.3847/1538-4357/aac9c4
[38] Ruiz-Lapuente, P., Comeron, F., Méndez, J., et al. 2004, Nature, 431, 1069.
doi:10.1038/nature03006
[39] Pilar Ruiz–Lapuente, 2019, New Astronomy Reviews, 85, 101523
[40] Schaefer,
B.
E.
&
Pagnotta,
A.
2012,
Nature,
481,
164.
doi:10.1038/nature10692
[41] Schmidt, B. P., Suntzeff, N. B., Phillips, M. M., et al. 1998, ApJ, 507, 46
[42] Timmes, F. X. & Swesty, F. D. 2000, ApJS, 126, 501
[43] Timmes, F. X. & Arnett, D. 1999, ApJS, 125, 277
[44] Turk, M. J., Smith, B. D., Oishi, J. S., et al. 2011, ApJS, 192, 9
[45] Wheeler, J. C., Harkness, R. P. 1990, Reports on Progress in Physics, 53,
1467
[46] Whelan, J. & Iben, I. 1973, ApJ, 186, 1007.
[47] Iben, I. & Tutukov, A. V. 1984, ApJS, 54, 335. doi:10.1086/190932
[48] Webbink, R. F. 1984, ApJ, 277, 355. doi:10.1086/161701
[49] Yoon, S.-C. & Langer, N. 2005, A&A, 435, 967. doi:10.1051/0004-
6361:20042542
[50] Yoon, S.-C. & Langer, N. 2004, A&A, 419, 623. doi:10.1051/0004-
6361:20035822