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10 results on '"Shafter, A.W."'

1. A recurrent nova super-remnant in the Andromeda galaxy

Author

Darnley, M.J., Hounsell, R., O’Brien, T.J., Henze, M., Rodríguez-Gil, P., Shafter, A.W., Shara, M.M., Vaytet, N.M.H., Bode, M.F., Ciardullo, R., Davis, B.D., Galera-Rosillo, R., Harman, D.J., Harvey, E.J., Healy, M.W., Ness, J.-U., Ribeiro, V.A.R.M., Williams, S.C., Darnley, M.J., Hounsell, R., O’Brien, T.J., Henze, M., Rodríguez-Gil, P., Shafter, A.W., Shara, M.M., Vaytet, N.M.H., Bode, M.F., Ciardullo, R., Davis, B.D., Galera-Rosillo, R., Harman, D.J., Harvey, E.J., Healy, M.W., Ness, J.-U., Ribeiro, V.A.R.M., and Williams, S.C.

Abstract

The accretion of hydrogen onto a white dwarf star ignites a classical nova eruption(1,2)-a thermonuclear runaway in the accumulated envelope of gas, leading to luminosities up to a million times that of the Sun and a high-velocity mass ejection that produces a remnant shell (mainly consisting of insterstellar medium). Close to the upper mass limit of a white dwarf(3) (1.4 solar masses), rapid accretion of hydrogen (about 10(-7) solar masses per year) from a stellar companion leads to frequent eruptions on timescales of years(4,5) to decades(6). Such binary systems are known as recurrent novae. The ejecta of recurrent novae, initially moving at velocities of up to 10,000 kilometres per second(7), must 'sweep up' the surrounding interstellar medium, creating cavities in space around the nova binary. No remnant larger than one parsec across from any single classical or recurrent nova eruption is known(8-10), but thousands of successive recurrent nova eruptions should be capable of generating shells hundreds of parsecs across. Here we report that the most frequently recurring nova, M31N 2008-12a in the Andromeda galaxy (Messier 31 or NGC 224), which erupts annually(11), is indeed surrounded by such a super-remnant with a projected size of at least 134 by 90 parsecs. Larger than almost all known remnants of even supernova explosions(12), the existence of this shell demonstrates that the nova M31N 2008-12a has erupted with high frequency for millions of years.

Published
2019

2. A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption (Corrigendum)

Author

Darnley, M.J., Henze, M., Steele, I.A., Bode, M.F., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Williams, S.C., Baer, D., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Kiyota, S., Kučáková, H., Maehara, H., Ness, J.-U., Piascik, A.S., Sala, G., Skillen, I., Smith, R.J., Wolf, M., Darnley, M.J., Henze, M., Steele, I.A., Bode, M.F., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Williams, S.C., Baer, D., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Kiyota, S., Kučáková, H., Maehara, H., Ness, J.-U., Piascik, A.S., Sala, G., Skillen, I., Smith, R.J., and Wolf, M.

Abstract

Contains fulltext : 159680.pdf (preprint version ) (Open Access)

Published
2016

3. M31N 2008-12a - The Remarkable Recurrent Nova in M31: Panchromatic Observations of the 2015 Eruption

Author

Darnley, M.J., Henze, M., Bode, M.F., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Ness, J.-U., Osborne, J.P., Page, K.L., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Shara, M.M., Steele, I.A., Williams, S.C., Arai, A., Arcavi, I., Barsukova, E.A., Boumis, P., Chen, T., Fabrika, S., Figueira, J., Gao, X., Gehrels, N., Godon, P., Goranskij, V.P., Harman, D.J., Hartmann, D.H., Hosseinzadeh, G., Horst, J.C., Itagaki, K., José, J., Kabashima, F., Kaur, A., Kawai, N., Kennea, J.A., Kiyota, S., Kučáková, H., Lau, K.M., Maehara, H., Naito, H., Nakajima, K., Nishiyama, K, O'Brien, T.J., Quimby, R., Sala, G., Sano, Y., Sion, E.M., Valeev, A.F., Watanabe, F., Watanabe, M., Williams, B.F., Xu, Z., Darnley, M.J., Henze, M., Bode, M.F., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Ness, J.-U., Osborne, J.P., Page, K.L., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Shara, M.M., Steele, I.A., Williams, S.C., Arai, A., Arcavi, I., Barsukova, E.A., Boumis, P., Chen, T., Fabrika, S., Figueira, J., Gao, X., Gehrels, N., Godon, P., Goranskij, V.P., Harman, D.J., Hartmann, D.H., Hosseinzadeh, G., Horst, J.C., Itagaki, K., José, J., Kabashima, F., Kaur, A., Kawai, N., Kennea, J.A., Kiyota, S., Kučáková, H., Lau, K.M., Maehara, H., Naito, H., Nakajima, K., Nishiyama, K, O'Brien, T.J., Quimby, R., Sala, G., Sano, Y., Sion, E.M., Valeev, A.F., Watanabe, F., Watanabe, M., Williams, B.F., and Xu, Z.

Abstract

Contains fulltext : 164095.pdf (preprint version ) (Open Access)

Published
2016

5. A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption

Author

Darnley, M.J., Henze, M., Steele, I.A., Bode, M.F., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Williams, S.C., Baer, D., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Kiyota, S., Kučáková, H., Maehara, H., Ness, J.-U., Piascik, A.S., Sala, G., Skillen, I., Smith, R.J., Wolf, M., Darnley, M.J., Henze, M., Steele, I.A., Bode, M.F., Ribeiro, V.A.R.M., Rodríguez-Gil, P., Shafter, A.W., Williams, S.C., Baer, D., Hachisu, I., Hernanz, M., Hornoch, K., Hounsell, R., Kato, M., Kiyota, S., Kučáková, H., Maehara, H., Ness, J.-U., Piascik, A.S., Sala, G., Skillen, I., Smith, R.J., and Wolf, M.

Abstract

Contains fulltext : 143734.pdf (preprint version ) (Open Access)

Published
2015

7. X-ray binaries: three topics

Author

van Paradijs, J.A., Shafter, A.W., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Published
1994

8. DO Leonis - a new eclipsing cataclysmic variable

Author

Abbott, T.M.C., Shafter, A.W., Wood, J.H., Tomaney, A.B., Haswell, Carole, Abbott, T.M.C., Shafter, A.W., Wood, J.H., Tomaney, A.B., and Haswell, Carole

Abstract

Photometric and spectroscopic observations of DO Leo have been obtained using the McDonald Observatory high-speed CCD photometer and a conventional two-channel photoelectric photometer. The data reveal eclipses that are approximately 1.5 m deep. A total of nine eclipses were observed in February and March 1988 and in April 1989. These data were used to establish an orbital period of 0.2345147(2) d. A low-resolution optical spectrum reveals significant He II 4686 emission in addition to the characteristic Balmer and He I emission lines.

9. DO Leonis: a new eclipsing cataclysmic variable

Author

Abbott, T.M.C., Shafter, A.W., Wood, J.H., Tomaney, A.B., Haswell, Carole, Abbott, T.M.C., Shafter, A.W., Wood, J.H., Tomaney, A.B., and Haswell, Carole

Abstract

Photometric and spectroscopic observations of DO Leo have been obtained using the McDonald Observatory high-speed CCD photometer and a conventional two-channel photoelectric photometer. The data reveal eclipses that are approximately 1.5 m deep. A total of nine eclipses were observed in February and March 1988 and in April 1989. These data were used to establish an orbital period of 0.2345147(2) d. A low-resolution optical spectrum reveals significant He II 4686 emission in addition to the characteristic Balmer and He I emission lines.

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