XMM-Newton detection of the 2.1 ms coherent pulsations from IGR J17379–3747

Simona Michela Mazzola, Rosario Iaria, Tiziana Di Salvo, Riggio, Bozzo, Sanna, D’Amico, Burderi, Papitto, Ferrigno

Risultato della ricerca: Article

6 Citazioni (Scopus)

Abstract

We report the detection of X-ray pulsations at 2.1 ms from the known X-ray burster IGR J17379-3747 using XMM-Newton. The coherent signal shows a clear Doppler modulation from which we estimate an orbital period of similar to 1.9 h and a projected semi-major axis of similar to 8 lt-ms. Taking into account the lack of eclipses (inclination angle of <75 degrees) and assuming a neutron star mass of 1.4 M-circle dot, we have estimated a minimum companion star of similar to 0.06 M-circle dot. Considerations on the probability distribution of the binary inclination angle make the hypothesis of a main-sequence companion star less likely. On the other hand, the close correspondence with the orbital parameters of the accreting millisecond pulsar SAX J1808.4-3658 suggests the presence of a bloated brown dwarf. The energy spectrum of the source is well described by a soft disk black-body component (kT similar to 0.45 keV) plus a Comptonisation spectrum with photon index similar to 1.9. No sign of emission lines or reflection components are significantly detected. Finally, combining the source ephemerides estimated from the observed outbursts, we obtained a first constraint on the long-term orbital evolution of the order of. P-orb = (-2.5 +/- 2.3) x 10(-12) s s(-1).
Lingua originaleEnglish
pagine (da-a)L17-
Numero di pagine5
RivistaASTRONOMY &amp; ASTROPHYSICS
Volume616
Stato di pubblicazionePublished - 2018

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XMM-Newton telescope
newton
companion stars
orbitals
inclination
outburst
ephemerides
main sequence stars
eclipses
pulsars
neutron stars
energy spectra
x rays
energy
modulation
photons
estimates
detection
distribution
index

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

XMM-Newton detection of the 2.1 ms coherent pulsations from IGR J17379–3747. / Mazzola, Simona Michela; Iaria, Rosario; Di Salvo, Tiziana; Riggio; Bozzo; Sanna; D’Amico; Burderi; Papitto; Ferrigno.

In: ASTRONOMY &amp; ASTROPHYSICS, Vol. 616, 2018, pag. L17-.

Risultato della ricerca: Article

Mazzola, SM, Iaria, R, Di Salvo, T, Riggio, Bozzo, Sanna, D’Amico, Burderi, Papitto & Ferrigno 2018, 'XMM-Newton detection of the 2.1 ms coherent pulsations from IGR J17379–3747', ASTRONOMY &amp; ASTROPHYSICS, vol. 616, pagg. L17-.
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title = "XMM-Newton detection of the 2.1 ms coherent pulsations from IGR J17379–3747",
abstract = "We report the detection of X-ray pulsations at 2.1 ms from the known X-ray burster IGR J17379-3747 using XMM-Newton. The coherent signal shows a clear Doppler modulation from which we estimate an orbital period of similar to 1.9 h and a projected semi-major axis of similar to 8 lt-ms. Taking into account the lack of eclipses (inclination angle of <75 degrees) and assuming a neutron star mass of 1.4 M-circle dot, we have estimated a minimum companion star of similar to 0.06 M-circle dot. Considerations on the probability distribution of the binary inclination angle make the hypothesis of a main-sequence companion star less likely. On the other hand, the close correspondence with the orbital parameters of the accreting millisecond pulsar SAX J1808.4-3658 suggests the presence of a bloated brown dwarf. The energy spectrum of the source is well described by a soft disk black-body component (kT similar to 0.45 keV) plus a Comptonisation spectrum with photon index similar to 1.9. No sign of emission lines or reflection components are significantly detected. Finally, combining the source ephemerides estimated from the observed outbursts, we obtained a first constraint on the long-term orbital evolution of the order of. P-orb = (-2.5 +/- 2.3) x 10(-12) s s(-1).",
author = "Mazzola, {Simona Michela} and Rosario Iaria and {Di Salvo}, Tiziana and Riggio and Bozzo and Sanna and D’Amico and Burderi and Papitto and Ferrigno",
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TY - JOUR

T1 - XMM-Newton detection of the 2.1 ms coherent pulsations from IGR J17379–3747

AU - Mazzola, Simona Michela

AU - Iaria, Rosario

AU - Di Salvo, Tiziana

AU - Riggio, null

AU - Bozzo, null

AU - Sanna, null

AU - D’Amico, null

AU - Burderi, null

AU - Papitto, null

AU - Ferrigno, null

PY - 2018

Y1 - 2018

N2 - We report the detection of X-ray pulsations at 2.1 ms from the known X-ray burster IGR J17379-3747 using XMM-Newton. The coherent signal shows a clear Doppler modulation from which we estimate an orbital period of similar to 1.9 h and a projected semi-major axis of similar to 8 lt-ms. Taking into account the lack of eclipses (inclination angle of <75 degrees) and assuming a neutron star mass of 1.4 M-circle dot, we have estimated a minimum companion star of similar to 0.06 M-circle dot. Considerations on the probability distribution of the binary inclination angle make the hypothesis of a main-sequence companion star less likely. On the other hand, the close correspondence with the orbital parameters of the accreting millisecond pulsar SAX J1808.4-3658 suggests the presence of a bloated brown dwarf. The energy spectrum of the source is well described by a soft disk black-body component (kT similar to 0.45 keV) plus a Comptonisation spectrum with photon index similar to 1.9. No sign of emission lines or reflection components are significantly detected. Finally, combining the source ephemerides estimated from the observed outbursts, we obtained a first constraint on the long-term orbital evolution of the order of. P-orb = (-2.5 +/- 2.3) x 10(-12) s s(-1).

AB - We report the detection of X-ray pulsations at 2.1 ms from the known X-ray burster IGR J17379-3747 using XMM-Newton. The coherent signal shows a clear Doppler modulation from which we estimate an orbital period of similar to 1.9 h and a projected semi-major axis of similar to 8 lt-ms. Taking into account the lack of eclipses (inclination angle of <75 degrees) and assuming a neutron star mass of 1.4 M-circle dot, we have estimated a minimum companion star of similar to 0.06 M-circle dot. Considerations on the probability distribution of the binary inclination angle make the hypothesis of a main-sequence companion star less likely. On the other hand, the close correspondence with the orbital parameters of the accreting millisecond pulsar SAX J1808.4-3658 suggests the presence of a bloated brown dwarf. The energy spectrum of the source is well described by a soft disk black-body component (kT similar to 0.45 keV) plus a Comptonisation spectrum with photon index similar to 1.9. No sign of emission lines or reflection components are significantly detected. Finally, combining the source ephemerides estimated from the observed outbursts, we obtained a first constraint on the long-term orbital evolution of the order of. P-orb = (-2.5 +/- 2.3) x 10(-12) s s(-1).

UR - http://hdl.handle.net/10447/296917

M3 - Article

VL - 616

SP - L17-

JO - ASTRONOMY &amp; ASTROPHYSICS

JF - ASTRONOMY &amp; ASTROPHYSICS

SN - 0004-6361

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