OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE

doi:https://doi.org/10.1088/0004-637X/812/1/63

Title: OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE

Full Record
Other Related Research

Abstract

We used ultra-deep UV observations obtained with the Hubble Space Telescope to search for optical companions to binary millisecond pulsars (MSPs) in the globular cluster 47 Tucanae. We identified four new counterparts (to MSPs 47TucQ, 47TucS, 47TucT, and 47TucY) and confirmed those already known (to MSPs 47TucU and 47TucW). In the color–magnitude diagram, the detected companions are located in a region between the main sequence and the CO white dwarf (WD) cooling sequences, consistent with the cooling tracks of He WDs with masses between 0.15 M{sub ⊙} and 0.20 M{sub ⊙}. For each identified companion, mass, cooling age, temperature, and pulsar mass (as a function of the inclination angle) have been derived and discussed. For 47TucU we also found that the past accretion history likely proceeded at a sub-Eddington rate. The companion to the redback 47TucW is confirmed to be a non-degenerate star, with properties particularly similar to those observed for black widow systems. Two stars have been identified within the 2σ astrometric uncertainty from the radio positions of 47TucH and 47TucI, but the available data prevent us from firmly assessing whether they are the true companions of these two MSPs.

Authors:

Cadelano, M.; Pallanca, C.; Ferraro, F. R.; Dalessandro, E.; Lanzoni, B. ^[1]; Salaris, M. ^[2]; Freire, P. C. C. ^[3]

Dipartimento di Fisica e Astronomia, Università di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna (Italy)
Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom)
Max-Planck-Institute für Radioastronomie, D-53121 Bonn (Germany)

Publication Date:: 2015-10-10

OSTI Identifier:: 22525262

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 812; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BINARY STARS; CARBON MONOXIDE; COLOR; COOLING; DIAGRAMS; INCLINATION; MASS; PULSARS; SPACE; TELESCOPES; WHITE DWARF STARS

Citation Formats


                    Cadelano, M., Pallanca, C., Ferraro, F. R., Dalessandro, E., Lanzoni, B., Salaris, M., and Freire, P. C. C. OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE.  United States: N. p., 2015. 
        Web.  doi:10.1088/0004-637X/812/1/63.

Copy to clipboard


                    Cadelano, M., Pallanca, C., Ferraro, F. R., Dalessandro, E., Lanzoni, B., Salaris, M., & Freire, P. C. C. OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE.  United States.  https://doi.org/10.1088/0004-637X/812/1/63

Copy to clipboard


                    Cadelano, M., Pallanca, C., Ferraro, F. R., Dalessandro, E., Lanzoni, B., Salaris, M., and Freire, P. C. C. Sat .  
        "OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE".  United States.  https://doi.org/10.1088/0004-637X/812/1/63.

Copy to clipboard


                    
@article{osti_22525262,

  title        = {OPTICAL IDENTIFICATION OF He WHITE DWARFS ORBITING FOUR MILLISECOND PULSARS IN THE GLOBULAR CLUSTER 47 TUCANAE},

  author       = {Cadelano, M. and Pallanca, C. and Ferraro, F. R. and Dalessandro, E. and Lanzoni, B. and Salaris, M. and Freire, P. C. C.},

  abstractNote = {We used ultra-deep UV observations obtained with the Hubble Space Telescope to search for optical companions to binary millisecond pulsars (MSPs) in the globular cluster 47 Tucanae. We identified four new counterparts (to MSPs 47TucQ, 47TucS, 47TucT, and 47TucY) and confirmed those already known (to MSPs 47TucU and 47TucW). In the color–magnitude diagram, the detected companions are located in a region between the main sequence and the CO white dwarf (WD) cooling sequences, consistent with the cooling tracks of He WDs with masses between 0.15 M{sub ⊙} and 0.20 M{sub ⊙}. For each identified companion, mass, cooling age, temperature, and pulsar mass (as a function of the inclination angle) have been derived and discussed. For 47TucU we also found that the past accretion history likely proceeded at a sub-Eddington rate. The companion to the redback 47TucW is confirmed to be a non-degenerate star, with properties particularly similar to those observed for black widow systems. Two stars have been identified within the 2σ astrometric uncertainty from the radio positions of 47TucH and 47TucI, but the available data prevent us from firmly assessing whether they are the true companions of these two MSPs.},

  doi          = {10.1088/0004-637X/812/1/63},

  url          = {https://www.osti.gov/biblio/22525262},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 1,

  volume       = 812,

  place        = {United States},

  year         = {2015},

  month        = {10}

}

Copy to clipboard

Journal Article:

https://doi.org/10.1088/0004-637X/812/1/63

Other availability

Find in Google Scholar

Search WorldCat to find libraries that may hold this journal

Save / Share:

Export Metadata

Save to My Library

Similar records in OSTI.GOV collections:

FORMATION OF BLACK WIDOWS AND REDBACKS—TWO DISTINCT POPULATIONS OF ECLIPSING BINARY MILLISECOND PULSARS

Journal Article Chen, Hai-Liang ; Chen, Xuefei ; Han, Zhanwen ; ... - Astrophysical Journal

Eclipsing binary millisecond pulsars (MSPs; the so-called black widows and redbacks) can provide important information about accretion history, pulsar irradiation of their companion stars, and the evolutionary link between accreting X-ray pulsars and isolated MSPs. However, the formation of such systems is not well understood, nor the difference in progenitor evolution between the two populations of black widows and redbacks. Whereas both populations have orbital periods between 0.1 and 1.0 days, their companion masses differ by an order of magnitude. In this paper, we investigate the formation of these systems via the evolution of converging low-mass X-ray binaries by employingmore »« less
https://doi.org/10.1088/0004-637X/775/1/27
FORMATION OF BINARY MILLISECOND PULSARS BY ACCRETION-INDUCED COLLAPSE OF WHITE DWARFS UNDER WIND-DRIVEN EVOLUTION

Journal Article Ablimit, Iminhaji ; Li, Xiang-Dong - Astrophysical Journal

Accretion-induced collapse (AIC) of massive white dwarfs (WDs) has been proposed to be an important channel to form binary millisecond pulsars (MSPs). Recent investigations on thermal timescale mass transfer in WD binaries demonstrate that the resultant MSPs are likely to have relatively wide orbit periods (≳ 10 days). Here we calculate the evolution of WD binaries taking into account the excited wind from the companion star induced by X-ray irradiation of the accreting WD, which may drive rapid mass transfer even when the companion star is less massive than the WD. This scenario can naturally explain the formation of themore »« less
https://doi.org/10.1088/0004-637X/800/2/98
EVOLUTION OF TRANSIENT LOW-MASS X-RAY BINARIES TO REDBACK MILLISECOND PULSARS

Journal Article Jia, Kun ; Li, Xiang-Dong - Astrophysical Journal

Redback millisecond pulsars (MSPs; hereafter redbacks) are a subpopulation of eclipsing MSPs in close binaries. The formation processes of these systems are not clear. The three pulsars showing transitions between rotation- and accretion-powered states belong to both redbacks and transient low-mass X-ray binaries (LMXBs), suggesting a possible evolutionary link between them. Through binary evolution calculations, we show that the accretion disks in almost all LMXBs are subject to the thermal-viscous instability during certain evolutionary stages, and the parameter space for the disk instability covers the distribution of known redbacks in the orbital period—companion mass plane. We accordingly suggest that themore »« less
https://doi.org/10.1088/0004-637X/814/1/74
A METAL-RICH LOW-GRAVITY COMPANION TO A MASSIVE MILLISECOND PULSAR

Journal Article Kaplan, D. L. ; Bhalerao, V. B. ; Van Kerkwijk, M. H. ; ... - Astrophysical Journal

Most millisecond pulsars with low-mass companions are in systems with either helium-core white dwarfs or non-degenerate (''black widow'' or ''redback'') stars. A candidate counterpart to PSR J1816+4510 was identified by Kaplan et al. whose properties were suggestive of both types of companions although identical to neither. We have assembled optical spectroscopy of the candidate companion and confirm that it is part of the binary system with a radial velocity amplitude of 343 {+-} 7 km s{sup -1}, implying a high pulsar mass, M{sub psr}sin {sup 3} i = 1.84 {+-} 0.11 M{sub Sun }, and a companion mass M{sub c}more »« less
https://doi.org/10.1088/0004-637X/765/2/158
Discovery of a millisecond pulsar in the 5.4 day binary 3FGL J1417.5–4402: Observing the late phase of pulsar recycling

Journal Article Camilo, F. ; Halpern, J. P. ; Bogdanov, S. ; ... - Astrophysical Journal

In a search of the unidentified Fermi gamma-ray source 3FGL J1417.5–4402 with the Parkes radio telescope, we discovered PSR J1417–4402, a 2.66 ms pulsar having the same 5.4 day orbital period as the optical and X-ray binary identified by Strader et al. The existence of radio pulsations implies that the neutron star is currently not accreting. Substantial outflows from the companion render the radio pulsar undetectable for more than half of the orbit, and may contribute to the observed Hα emission. Our initial pulsar observations, together with the optically inferred orbit and inclination, imply a mass ratio of 0.171 ± 0.002, a companion massmore »« less
https://doi.org/10.3847/0004-637X/820/1/6

Similar Records