arXiv:astro-ph/0406263v1 10 Jun 2004
Frontier in Astroparticle Physics and Cosmology
Circumstellar Interaction of Type Ia Supernova SN 2002ic
Ken’ichi NOMOTO, Tomoharu SUZUKI, Jinsong DENG, Tatsuhiro UENISHI
Department of Astronomy & Research Center for the Early Universe, School of
Science, University of Tokyo, Tokyo 113-0033, Japan
Institute of Earth Science and Astronomy, University of Tokyo, Meguro–ku,
Osservatorio Astronomico di Trieste, via G.B.& Tiepolo 11, I-34131 Trieste, Italy
SN 2002ic is a unique supernova which shows the typical spectral features
of Type Ia supernovae (SNe Ia) near maximum light, but also apparent hydrogen
features that have been absent in SNe Ia. We have calculated hydrodynamical
models for the interaction between the SN Ia ejecta and the H-rich circumstellar
medium (CSM) to reproduce the observed features of SN 2002ic. Based on our
modeling, we suggest that CSM is aspherical (or highly clumpy) and contains ∼
4-5 M⊙. Possible progenitor systems of SN 2002ic are discussed.
1. Type Ia Supernovae and Circumstellar Medium
Type Ia supernovae (SNe Ia) are characterized by the lack of hydrogen and
the prominent Si line in their spectra near maximum light and widely believed
to be thermonuclear explosions of mass-accreting white dwarfs in binary systems.
SNe Ia have been used as a “standard candle” to determine cosmological param-
eters thanks to their relatively uniform light curves and spectral evolution. SNe
Ia are also the major sources of Fe in the galactic and cosmic chemical evolution.
Despite such importance, the immediate progenitor binary systems have not been
clearly identified yet (e.g., [10, 13]).
For a model of SN Ia progenitors, Hachisu et al. [5, 6] proposed a single
degenerate model in which the white dwarf blows a massive and fast wind (up
to 10−4M⊙yr−1and 2000 km s−1) and avoids a formation of common envelope
when the mass transfer rate from the normal companion exceeds a critical rate of
∼ 1 × 10−6M⊙yr−1. Such an evolutionary phase is dubbed “accretion wind
evolution” instead of “common envelope evolution.” Such a binary can keep its
c ?2004 by Universal Academy Press, Inc.
Furthermore, the white dwarf wind collides with the companion and strips heavily
off its surface matter. This stripping rate reaches a few or several times the wind
mass loss rate of the white dwarf, i.e., ∼ 1×10−4M⊙yr−1or more . The matter
stripped off has a much lower velocity than the white dwarf wind itself and forms
an excretion disk around the binary. Thus the model predict the coexistence of a
fast white dwarf wind blowing mainly in the pole direction and a massive disk or
a torus around the binary. Deng et al.  propose a new classification, Type IIa
supernovae, for these events.
 Branch, D., Livio, M., Yungelson, L. R., Roffi, F. R., & Baron, E. 1995,
PASP 107, 717
 Chugai, N. N., & Yungelson, L. R. 2004, Astronomy Letters 30, 65
 Deng, J., Kawabata, K. S., Ohyama, Y., Nomoto, K., Mazzali, P., Wang, L.,
Jeffery, D. J. Iye, M., Tomita, H., & Yoshii, Y., 2004, ApJ 605, L37
 Germany, L. M., Reiss, D. J., Sadler, E. M., Schmidt, B. P., & Stubbs, C.
W. 2000, ApJ 533, 320
 Hachisu, I., Kato, M., & Nomoto, K. 1999a, ApJ 522, 487
 Hachisu, I., Kato, M., Nomoto, K., & Umeda, H. 1999b, ApJ 519, 314
 Hachisu, I., & Kato, M. 2004, ApJ 590, 445
 Hamuy, M., et al. 2003, Nature 424, 651
 Livio, M., & Riess, A. G. 2003, ApJ 594, L93
 Lundqvist, P., Sollerman, J., Leibundgut, B., Baron, E., Fransson, C., &
Nomoto, K. 2003, in From Twilight to Highlight: The Physics of Supernovae,
ed. W. Hillebrandt & B. Leibundgut (Berlin: Springer), 309
 Nomoto, K. 1982, ApJ 253, 798
 Nomoto, K., Thielemann, F.-K., & Yokoi, K. 1984, ApJ 268, 644
 Nomoto, K., et al. 2000, in Type Ia Supernovae: Theory and Cosmolgy, eds.
J. Niemeyer & J. Truran (Cambridge: Cambridge Univ. Press), 63
 Rigon, L., et al. 2003, MNRAS 340, 191
 Schlegel, D.J., Finkbeiner, D.P., Davis, M., 1998, ApJ 500, 525
 Suzuki, T., & Nomoto, K., 1995, ApJ 455, 658
 Turatto, M., Mazzali, P.A., Young,T.R., Nomoto, K., et al. 1998, ApJ 498,
 Wang, L., Baade, D., H¨ oflich, Wheeler, J. C., Kawabata, K., & Nomoto, K.
2004, ApJ 604, L53
 Wood-Vasey, W. M., et al. 2002, IAUC, 8019