Properties of the redback millisecond pulsar binary 3FGL J0212.1+5320

Shahbaz, T.; Linares, M.; Breton, R. P.

doi:10.1093/mnras/stx2195

Cited by 29 publications

(36 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using UVESPOP spectra we find that the line strength versus temperature relation of the metallic absorption lines in the 6000-6500 Å spectral range decreases with increasing temperature. Similarly, for the Hα absorption-line (Balmer), we find that the line strength increases with increasing temperature (Shahbaz et al 2017;Linares et al 2018). Therefore, we can compute the secondary star's metallic (K 2,Z ) or Balmer (K 2,H ) absorption-line radial velocity semi-amplitude.…”

Section: The Pulsar-state Radial Velocity Curvementioning

confidence: 69%

“…The moderate inclination angle of 54 • of the system (McConnell et al 2015) implies that the contrast between the observed spectral type at different orbital phases is reduced, which means that the observer always sees the heated inner face of the secondary star and thus the true spectral type of the secondary star is cooler. Simultaneous modelling of the optical light-and radial-velocity curves during the pulsar-state should reveal the true spectral type of the secondary star (Shahbaz et al 2017;Linares et al 2018)…”

Section: Spectral Type Changes Along the Orbitmentioning

confidence: 99%

See 1 more Smart Citation

The binary millisecond pulsar PSR J1023+0038 – II. Optical spectroscopy

Shahbaz

Linares

Rodríguez‐Gil

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present time-resolved optical spectroscopy of the "redback" binary millisecond pulsar system PSR J1023+0038 during both its radio pulsar (2009) and accretion disc states (2014 and 2016). We provide observational evidence for the companion star being heated during the disc-state. We observe a spectral type change along the orbit, from ∼G5 to ∼F6 at the secondary star's superior and inferior conjunction, respectively, and find that the corresponding irradiating luminosity can be powered by the high energy accretion luminosity or the spin down luminosity of the neutron star. We determine the secondary star's radial velocity semi-amplitude from the metallic (primarily Fe and Ca) and Hα absorption lines during these different states. The metallic and Hα radial velocity semi-amplitude determined from the 2009 pulsar-state observations allows us to constrain the secondary star's true radial velocity K 2 =276.3±5.6 km s −1 and the binary mass ratio q=0.137±0.003. By comparing the observed metallic and Hα absorption-line radial velocity semi-amplitudes with model predictions, we can explain the observed semi-amplitude changes during the pulsar-state and during the pulsar/disc-state transition as being due to different amounts of heating and the presence of an accretion disc, respectively.

show abstract

Section: The Pulsar-state Radial Velocity Curvementioning

confidence: 69%

Section: Spectral Type Changes Along the Orbitmentioning

confidence: 99%

The binary millisecond pulsar PSR J1023+0038 – II. Optical spectroscopy

Shahbaz

Linares

Rodríguez‐Gil

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…The model, described in the following, has been successfully applied to LCs and RVCs of neutron star and black hole X-ray binaries (see Shahbaz et al 2000Shahbaz et al , 2003Shahbaz et al , 2017 for more details).…”

Section: Modelingmentioning

confidence: 99%

“…In determining the binary parameters, we use a Markov chain Monte Carlo (MCMC) method convolved with a differential evolution fitting algorithm (see Vrugt 2016;Shahbaz et al 2017). We use a Bayesian framework to determine our binary model parameters (Gregory 2005).…”

Section: Binary Parameters and Irradiationmentioning

confidence: 99%

Peering into the Dark Side: Magnesium Lines Establish a Massive Neutron Star in PSR J2215+5135

Linares

Shahbaz

Casares

2018

ApJ

Self Cite

335

237

View full text Add to dashboard Cite

New millisecond pulsars (MSPs) in compact binaries provide a good opportunity to search for the most massive neutron stars. Their main-sequence companion stars are often strongly irradiated by the pulsar, displacing the effective center of light from their barycenter and making mass measurements uncertain. We present a series of optical spectroscopic and photometric observations of PSRJ2215+5135, a "redback" binary MSP in a 4.14hr orbit, and measure a drastic temperature contrast between the dark/cold (T N =5660 -+ 380470 K) sides of the companion star. We find that the radial velocities depend systematically on the atmospheric absorption lines used to measure them. Namely, the semi-amplitude of the radial velocity curve (RVC) of J2215 measured with magnesium triplet lines is systematically higher than that measured with hydrogen Balmer lines, by 10%. We interpret this as a consequence of strong irradiation, whereby metallic lines dominate the dark side of the companion (which moves faster) and Balmer lines trace its bright (slower) side. Further, using a physical model of an irradiated star to fit simultaneously the two-species RVCs and the three-band light curves, we find a center-of-mass velocity of K 2 =412.3±5.0 km s −1 and an orbital inclination i=63°.

show abstract

“…At each phase of the model, we take the intensity-weighted velocity offset of each grid element from the center of mass as viewed by an observer, and combine it with an effective temperature-equivalent width relation for Mgb taken from Johansson et al (2010). This method is similar to that used by Shahbaz et al (2017) except that we do not set the equivalent widths of the elements heated beyond a certain point to zero, since this is not demanded by the data. Future spectroscopy with a larger telescope would allow improvements in the quality of the spectra that could show the need for additional modeling.…”

Section: Modeling the Radial Velocitiesmentioning

confidence: 99%

A New Likely Redback Millisecond Pulsar Binary with a Massive Neutron Star: 4FGL J2333.1–5527

Swihart

Strader

Urquhart

et al. 2020

ApJ

View full text Add to dashboard Cite

We present the discovery of a likely new redback millisecond pulsar binary associated with the Fermi γ-ray source 4FGL J2333.1-5527. Using optical photometric and spectroscopic observations from the SOAR telescope, we identify a low-mass, main sequence-like companion in a 6.9-hr, highly inclined orbit around a suspected massive neutron star primary. Archival XMM-Newton X-ray observations show this system has a hard power-law spectrum Γ = 1.6 ± 0.3 and L X ∼ 5 × 10 31 erg s −1 , consistent with redback millisecond pulsar binaries. Our data suggest that for secondary masses typical of redbacks, the mass of the neutron star is likely well in excess of ∼ 1.4 M , but future timing of the radio pulsar is necessary to bolster this tentative conclusion. This work shows that a bevy of nearby compact binaries still await discovery, and that unusually massive neutron stars continue to be common in redbacks.

show abstract

Properties of the redback millisecond pulsar binary 3FGL J0212.1+5320

Cited by 29 publications

References 61 publications

The binary millisecond pulsar PSR J1023+0038 – II. Optical spectroscopy

The binary millisecond pulsar PSR J1023+0038 – II. Optical spectroscopy

Peering into the Dark Side: Magnesium Lines Establish a Massive Neutron Star in PSR J2215+5135

A New Likely Redback Millisecond Pulsar Binary with a Massive Neutron Star: 4FGL J2333.1–5527

Contact Info

Product

Resources

About