Hiding in Plain Sight: Chandra Observations of the Quiescent Neutron Star 4U 2129+47 in Eclipse

@article{Nowak2002HidingIP,
  title={Hiding in Plain Sight: Chandra Observations of the Quiescent Neutron Star 4U 2129+47 in Eclipse},
  author={Michael A. Nowak and Sebastian Heinz and Mitchell C. Begelman},
  journal={The Astrophysical Journal},
  year={2002},
  volume={573},
  pages={778 - 788}
}
During a previous outburst phase, the neutron star 4U 2129+47 exhibited evidence for a spatially extended accretion disk corona via broad, partial X-ray eclipses occurring periodically on the 5.24 hr orbit. Since 1983, however, 4U 2129+47 has entered a quiescent state several orders of magnitude fainter. We have performed a 37 ks (≈two binary orbits) Chandra observation of 4U 2129+47 to determine whether an extended coronal structure also exists in quiescence. Total eclipses are found, and the… 

A FURTHER DROP INTO QUIESCENCE BY THE ECLIPSING NEUTRON STAR 4U 2129+47

The low-mass X-ray binary 4U 2129+47 was discovered during a previous X-ray outburst phase and was classified as an accretion disk corona source. A 1% delay between two mid-eclipse epochs measured

X-ray eclipse time delays in 4U 2129+47

Aims. 4U 2129+47 was discovered in the early 80’s and classified as an accretion disk corona source due to its broad and partial X-ray eclipses. The 5.24 h binary orbital period was inferred from the

X-Ray Studies of Two Neutron Stars in 47 Tucanae: Toward Constraints on the Equation of State

We report spectral and variability analysis of two quiescent low-mass X-ray binaries (X5 and X7, previously detected with the ROSAT HRI) in a Chandra ACIS-I observation of the globular cluster 47

MS 1603.6+2600: an accretion disc corona source?

We have observed the eclipsing low-mass X-ray binary MS 1603.6+2600 with Chandra for 7 ks. The X-ray spectrum is well fit with a single absorbed power law with an index of ~2. We find a clear

A Chandra Observation of the Neutron Star X-Ray Transient and Eclipsing Binary MXB 1659–29 in Quiescence

After almost 2.5 yr of actively accreting, the neutron star X-ray transient and eclipsing binary MXB 1659-29 returned to quiescence in 2001 September. We report on a Chandra observation of this

On the Lack of Thermal Emission from the Quiescent Black Hole XTE J1118+480: Evidence for the Event Horizon

A soft component of thermal emission is very commonly observed from the surfaces of quiescent, accreting neutron stars. We searched with Chandra for such a surface component of emission from the

The Hard Quiescent Spectrum of the Neutron Star X-Ray Transient EXO 1745–248 in the Globular Cluster Terzan 5

We present a Chandra observation of the globular cluster Terzan 5 during times when the neutron star X-ray transient EXO 1745-248 located in this cluster was in its quiescent state. We detected the

The Evolution of the High-Energy Tail in the Quiescent Spectrum of the Soft X-Ray Transient Aquila X-1

A moderate level of variability has been detected in the quiescent luminosity of several neutron star soft X-ray transients. Spectral variability was first revealed by Chandra observations of Aql X-1

FURTHER CONSTRAINTS ON THERMAL QUIESCENT X-RAY EMISSION FROM SAX J1808.4-3658

We observed SAX J1808.4-3658 (1808), the first accreting millisecond pulsar, in deep quiescence with XMM-Newton and (near simultaneously) Gemini-South. The X-ray spectrum of 1808 is similar to that

Variable Thermal Emission from Aquila X-1 in Quiescence

We obtained four Chandra/ACIS-S observations beginning 2 weeks after the end of the 2000 November outburst of the neutron star (NS) transient Aql X-1. Over the 5 month span in quiescence, the X-ray

References

SHOWING 1-10 OF 40 REFERENCES

Accretion Disk Coronae

Recent observations of partial X-ray eclipses from 4U 1822-37 have shown that the central X-ray source in this system is diffused by a large Compton-thick accretion disk corona (ADC). We show that

A Chandra Observation of the Globular Cluster Terzan 1: The Neutron Star X-Ray Transient X1732–304 in Quiescence

We present a short (~3.6 ks) Chandra/HRC-I observation of the globular cluster Terzan 1. This cluster is known to contain the bright neutron star low-mass X-ray binary X1732-304, which was active

X-ray emission from 4U 2129+47 (= V1727 Cygni) in quiescence

Observations with the ROSAT HRI allow detection of weak X-ray flux from the low-mass X-ray binary (LMXB) 4U 2129+47 during its current quiescent state. The quiescent luminosity is similar to that

ASCA Observations of Transient X-Ray Sources in Quiescence

Soft X-ray transients are most probably low-mass binary systems containing either a neutron star (NS-LMXB) or a black hole (BH-LMXB). We have systematically investigated thirteen soft X-ray

A Method for Distinguishing between Transiently Accreting Neutron Stars and Black Holes, in Quiescence

Neutron stars and black holes often reside in binaries where the accretion rate onto the compact object varies by orders of magnitude. These "X-ray transients" are observed both in outburst (when the

The Quiescent X-Ray Spectrum of the Neutron Star in Centaurus X-4 Observed with Chandra/ACIS-S

We report on spectral and intensity variability analysis from a Chandra/ACIS-S observation of the transient, type I X-ray bursting low-mass X-ray binary Cen X-4. The quiescent X-ray spectrum during

Black Hole and Neutron Star Transients in Quiescence

We consider the X-ray luminosity difference between neutron star and black hole soft X-ray transients (NS and BH SXTs) in quiescence. The current observational data suggest that BH SXTs are

Advection-dominated Accretion Model of the Black Hole V404 Cygni in Quiescence

We have analyzed archival ASCA data on the soft X-ray transient source V404 Cyg in quiescence. We find that in the energy range 0.7-8.5 keV the spectrum is a hard power law with a photon spectral

Discovery of an X-ray burst from 4U 2129 + 47

Einstein MPC observations of the 5.2-h binary 4U 2129 + 47 are analyzed, and a type 1 X-ray burst with rise time 6.5 + or 1.5 s, peak 2-10-keV flux about 1 nerg/sq cm s, and peak color temperature

On the Bolometric Quiescent Luminosity and Luminosity Swing of Black Hole Candidate and Neutron Star Low-Mass X-Ray Transients

Low-mass X-ray transients hosting black hole candidates display on average a factor of ~100 larger swing in the minimum (quiescent) to maximum (outburst) X-ray luminosity than neutron star systems