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34 results on '"Bode, M.F."'

4. 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

5. Radio observations of the classical nova Cygni 92 eighty days after outburst

Author

Pavelin, P.E., Davis, R.J., Morrison, L.V., Bode, M.F., and Ivison, R.J.

Subjects
Stars -- Structure, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

A subject of binary stellar systems results in classical novae, in which the thermonuclear processes on the surface of the white dwarf, a primary component, causes the causes eruption of stellar material. The radio emission noted in these ejections is a result of the thermal bremsstrahlung mechanism occurring within an isothermal, expanding shell of ionized gas. Nova Cygni 92 was observed through Multi-Element Radio Linked Interferometer Network (MERLIN) and its temperatures were calculated.

Published
1993

6. X-ray detection of Nova Herculis 1991 five days after optical outburst

Author

Lloyd, H.M., O'Brien, T.J., Bode, M.F., Predehl, P., Schmitt, J.H.M.M., Trumper, J., Watson, M.G., and Pounds, K.A.

Subjects
Stars, New -- Observations, X-ray astronomy -- Research, Environmental issues, Science and technology, Zoology and wildlife conservation
Published
1992

7. 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

8. 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

9. XMM-Newton X-ray and Ultraviolet Observations of the Fast Nova V2491 Cyg during the Supersoft Source Phase

Author

Ness, J.-U., Osborne, J.P., Dobrotka, A., Page, K.L., Drake, J.J., Pinto, C., Detmers, R.G., Schwarz, G., Bode, M.F., Beardmore, A.P., Starrfield, S., Hernanz, M., Sala, G., Krautter, J., Woodward, C.E., Astrophysics, and Sub High energy Astrophysics begr 1/1/15

Abstract

Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2 minutes after an extended factor of three decline lasting ∼3 hr, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves of the novae V4743 Sgr and RS Oph, as it occurred on the same timescale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for four intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of Oi and Ni are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blueshifts indicating an expansion velocity of 3000–3400 km s−1, which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743 Sgr and the symbiotic recurrent nova RS Oph are presented. The SSS spectrum of V4743 Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RS Oph are as narrow as in V2491 Cyg, but they are less blueshifted. A remarkable similarity in the continua of V2491 Cyg and RS Oph is found. The only differences are smaller line shifts and additional emission lines in RS Oph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05 Å, 29.45 Å, and 30.0Å. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required.

Published
2011

10. 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

13. XMM-Newton X-ray and Ultraviolet Observations of the Fast Nova V2491 Cyg during the Supersoft Source Phase

Author

Astrophysics, Sub High energy Astrophysics begr 1/1/15, Ness, J.-U., Osborne, J.P., Dobrotka, A., Page, K.L., Drake, J.J., Pinto, C., Detmers, R.G., Schwarz, G., Bode, M.F., Beardmore, A.P., Starrfield, S., Hernanz, M., Sala, G., Krautter, J., Woodward, C.E., Astrophysics, Sub High energy Astrophysics begr 1/1/15, Ness, J.-U., Osborne, J.P., Dobrotka, A., Page, K.L., Drake, J.J., Pinto, C., Detmers, R.G., Schwarz, G., Bode, M.F., Beardmore, A.P., Starrfield, S., Hernanz, M., Sala, G., Krautter, J., and Woodward, C.E.

Published
2011

14. A Planetary Nebula around Nova V458 Vulpeculae Undergoing Flash Ionization

Author

Wesson, R., Barlow, M.J., Corradi, R.L.M., Drew, J.E., Groot, P.J., Knigge, C., Steeghs, D., Gaensicke, B.T., Napiwotzki, R., Rodriguez-Gil, P., Zijlstra, A.A., Bode, M.F., Drake, J.J., Frew, D.J., Gonzalez-Solares, E.A., Greimel, R., Irwin, M.J., Morales-Rueda, L., Nelemans, G.A., Parker, Q.A., Sale, S.E., Sokoloski, J.L., Somero, A., Uthas, H., Walton, N.A., Warner, B., Watson, C.A., Wright, N.J., Wesson, R., Barlow, M.J., Corradi, R.L.M., Drew, J.E., Groot, P.J., Knigge, C., Steeghs, D., Gaensicke, B.T., Napiwotzki, R., Rodriguez-Gil, P., Zijlstra, A.A., Bode, M.F., Drake, J.J., Frew, D.J., Gonzalez-Solares, E.A., Greimel, R., Irwin, M.J., Morales-Rueda, L., Nelemans, G.A., Parker, Q.A., Sale, S.E., Sokoloski, J.L., Somero, A., Uthas, H., Walton, N.A., Warner, B., Watson, C.A., and Wright, N.J.

Abstract

Contains fulltext : 72738.pdf ( ) (Open Access) Contains fulltext : 72738.pdf (publisher's version ) (Closed access)

Published
2008

16. ARTEMiS (Automated Robotic Terrestrial Exoplanet Microlensing Search): A possible expert-system based cooperative effort to hunt for planets of Earth mass and below

Author

Dominik, M., primary, Horne, K., additional, Allan, A., additional, Rattenbury, N.J., additional, Tsapras, Y., additional, Snodgrass, C., additional, Bode, M.F., additional, Burgdorf, M.J., additional, Fraser, S.N., additional, Kerins, E., additional, Mottram, C.J., additional, Steele, I.A., additional, Street, R.A., additional, Wheatley, P.J., additional, and Wyrzykowski, Ł., additional

Published
2008
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21. HST /WFPC2 snapshot imaging of symbiotic stars.

Author

Brocksopp, C., Bode, M.F., and Eyres, S.P.S.

Subjects
*SYMBIOTIC stars, *STAR observations, *CIRCUMSTELLAR matter
Abstract

Presents the results of a Hubble Space Telescope (HST)/WFPC2 snapshot imaging survey of selected symbiotic stars in 1999/2000. Observation of seven sources in filters F218W; Presence of extended emission; Possible optical extension; Circumstellar matter; Radio images of HD 149427.

Published
2003
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22. The remnant of Nova Cassiopeiae 1993 (V705 Cassiopeiae).

Author

Eyres, S.P.S., Bode, M.F., O'Brien, T.J., Watson, S.K., and Davis, R.J.

Subjects
*RADIO sources (Astronomy), *CIRCUMSTELLAR matter
Abstract

We have detected radio emission from the remnant of V705 Cas, beginning 221 d after visual maximum. We follow the remnant from first detection while still optically thick through the turn-over to optically thin emission, and finally confirming the absence of emission due to expansion and fading by the end of 1998. While the emission is consistent with thermal bremsstrahlung, as seen in most previous novae, the small-scale structure shows two ridge-like features, which develop significantly from day 585 until our last detection on day 1544. While the development is fairly rapid, it is also much smoother than that seen in V1974 Cyg, in that we can follow individual features as they change over almost 1000 d. Our optical spectra unequivocally indicate some form of axial symmetry, as derived from the velocity structure. This is difficult to reconcile with the observed development in the radio images. We suggest a number of possible explanations. [ABSTRACT FROM AUTHOR]

Published
2000
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23. Colliding winds in V1016 Cygni.

Author

Watson, S.K., Eyres, S.P.S., Davis, R.J., Bode, M.F., Richards, A.M.S., and Kenny, H.T.

Subjects
SYMBIOTIC stars, BRIGHTNESS temperature
Abstract

We present MERLIN observations of the symbiotic nova V1016 Cygni made at 6 cm between 1992 and 1997 and at 18 cm in 1993 and 1997. In the 6-cm images we find complex structure which has not been previously seen, in particular three bright components. These components do not appear to be expanding as would be expected from the remains of a hot wind resulting from the nova outburst. The change in positions of two of the features exhibits tentative east–west movement. The brightness temperature of the peak with the highest flux density remains above 50 000 K in all epochs, thereby confirming the presence of shocked material in the system. At 18 cm there is no evidence of any non-thermal emission as might be expected from comparison with a sister star, HM Sge. [ABSTRACT FROM AUTHOR]

Published
2000
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24. High-resolution radio observations of HM Sge -- II. Two decades after outburst.

Author

Richards, A.M.S., Bode, M.F., Eyres, S.P.S., Kenny, H.T., Davis, R.J., and Watson, S.K.

Subjects
*BINARY stars, *STELLAR winds, *ASTRONOMICAL observations
Abstract

HM Sge is a symbiotic binary star that underwent a nova-like outburst in 1975. Its radio emission has been monitored using MERLIN and the VLA, and maps from 1992 to 1997 are presented. Thermal emission within 0.4 arcsec of the optical peak is elongated north--south and hotspots appear to be moving around an anticlockwise ellipse. If this is due to motion in an inclined disc, the period is ∼ 90 yr. Eyres et al. predicted that if this is due to Mach shocks in the post-nova wind, proper motions should be seen in expansion. This has not been detected since 1992, so an alternative model is adopted, based on the work of Eyres et al. and Kenny et al., of colliding winds in a binary system following the nova-like outburst. The emission peaks appear to be corotating with the binary orbit as the ionization front and the hot wind from the white dwarf interact with the Mira wind. The positions of the stars are estimated, at a separation of ∼ 25 au. A distance of ∼ 1 kpc is most consistent with the observations reported here. On arcsecond scales the emission is extended east--west, consistent with a biconical outflow arising from the collimation of the nova outburst through interaction with the pre-existing cool wind. The presence of non-thermal emission at a separation of ∼700 mas from the stars is confirmed. This is very unusual at such a distance from low-mass stars, and could arise from synchrotron emission in a μT magnetic field. A model for this is developed, which shows that non-thermal emission is expected to decline within decades as the nova wind decelerates. This could explain the non-detection of non-thermal emission in other symbiotic stars. [ABSTRACT FROM AUTHOR]

Published
1999
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