Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700-37
- Based on new Chandra X-ray telescope data, we present empirical evidence of plasma Compton cooling during a flare in the non-pulsating massive X-ray binary 4U1700-37. This behaviour might be explained by quasi-spherical accretion on to a slowly rotating magnetized neutron star (NS). In quiescence, the NS in 4U1700-37 is surrounded by a hot radiatively cooling shell. Its presence is supported by the detection of mHz quasi-periodic oscillations likely produced by its convection cells. The high plasma temperature and the relatively low X-ray luminosity observed during the quiescence, point to a small emitting area similar to 1 km, compatible with a hotspot on an NS surface. The sudden transition from a radiative to a significantly more efficient Compton cooling regime triggers an episode of enhanced accretion resulting in a flare. During the flare, the plasma temperature drops quickly. The predicted luminosity for such transitions, similar to 3 x 10(35) erg s(-1), is very close to the luminosity of 4U1700-37 during quiescence. TheBased on new Chandra X-ray telescope data, we present empirical evidence of plasma Compton cooling during a flare in the non-pulsating massive X-ray binary 4U1700-37. This behaviour might be explained by quasi-spherical accretion on to a slowly rotating magnetized neutron star (NS). In quiescence, the NS in 4U1700-37 is surrounded by a hot radiatively cooling shell. Its presence is supported by the detection of mHz quasi-periodic oscillations likely produced by its convection cells. The high plasma temperature and the relatively low X-ray luminosity observed during the quiescence, point to a small emitting area similar to 1 km, compatible with a hotspot on an NS surface. The sudden transition from a radiative to a significantly more efficient Compton cooling regime triggers an episode of enhanced accretion resulting in a flare. During the flare, the plasma temperature drops quickly. The predicted luminosity for such transitions, similar to 3 x 10(35) erg s(-1), is very close to the luminosity of 4U1700-37 during quiescence. The transition may be caused by the accretion of a clump in the stellar wind of the donor star. Thus, a magnetized NS nature of the compact object is strongly favoured.…
Verfasserangaben: | M. Martinez-Chicharro, J. M. Torrejon, Lida OskinovaORCiDGND, F. Furst, K. Postnov, J. J. Rodes-Roca, Rainer HainichGND, A. Bodaghee |
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DOI: | https://doi.org/10.1093/mnrasl/slx165 |
ISSN: | 0035-8711 |
ISSN: | 1365-2966 |
Titel des übergeordneten Werks (Englisch): | Monthly notices of the Royal Astronomical Society |
Verlag: | Oxford Univ. Press |
Verlagsort: | Oxford |
Publikationstyp: | Wissenschaftlicher Artikel |
Sprache: | Englisch |
Datum der Erstveröffentlichung: | 09.10.2017 |
Erscheinungsjahr: | 2018 |
Datum der Freischaltung: | 25.03.2022 |
Freies Schlagwort / Tag: | V*V884 Sco; X-rays: binaries; stars: individual: 4U1700-37 |
Band: | 473 |
Ausgabe: | 1 |
Seitenanzahl: | 5 |
Erste Seite: | L74 |
Letzte Seite: | L78 |
Fördernde Institution: | STScI award [44A-1096046]; MECD fellowship [PRX17/00114]; [ESP2014-53672-C3-3P] |
Organisationseinheiten: | Mathematisch-Naturwissenschaftliche Fakultät / Institut für Physik und Astronomie |
DDC-Klassifikation: | 5 Naturwissenschaften und Mathematik / 53 Physik / 530 Physik |
Peer Review: | Referiert |
Publikationsweg: | Open Access / Green Open-Access |