Constraining the Dense Matter Equation of State with Lynx...
Transcript of Constraining the Dense Matter Equation of State with Lynx...
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Constraining the Dense Matter Equation of State
with Lynx Observations of Globular Cluster X-ray Binaries
Slavko Bogdanov
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The interior structure of neutron stars is unknown
?
Outer crust
Inner crust
Outer core
Inner core
Atmosphere
~11 km (~41014 g cm3)
0.5 km (21014 g cm3) – nuclear density0.1 km (41011 g cm3) – “neutron drip”
~12-15 km (~1015 g cm3)
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The state of cold, supranuclear matter is unknown
Hebeler et al. ApJ, 773, 11 (2013)
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The neutron star mass-radius relation
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Mapping between P- and M-R
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Mass measurements from radio pulsar timing- e.g. ~2M NSs; Demorest et al. Nature, 467, 1081 (2010); Antoniadis et al. Science, 340,
448 (2013)
Maximum spin rate of neutron stars- e.g. 716 Hz pulsar; Hessels et al. Science, 311, 1901 (2006)
kiloHertz quasi-periodic oscillations (QPOs)- e.g. Miller et al. ApJ, 509, 793 (1998)
Cooling rates of neutron stars- e.g. Page et al. NuPhA, 777, 497 (2006)
Photospheric radius expansion in thermonuclear bursts - Joss Nature, 270, 310 (1977); Özel et al. (2009); Steiner et al. (2010); etc…
Pulse profile/waveform/light curve modeling of accreting and “recycled” MSPs
- e.g., Pechenick et al. (1983); Poutanen & Gierlinski (2003); Bhattacharyya et al. (2005); Morsink & Leahy (2011); Bogdanov (2013); Lo et al. (2013); etc...
Radius measurements via X-ray spectroscopy of quiescent LMXBs
- e.g., Rutledge et al. (2001); Heinke et al. (2006,2014); Guillot et al. (2013); etc…
Observational methods for dense matterequation of state constraints using neutron stars
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Neutron Star Radius Measurements from Spectroscopy
Quiescent Low-Mass X-ray Binaries
• Flux measured by a distant observer:
Flat Schwarzschild
R (1+z) RNS
Blackbody
Hydrogenatmosphere
• Measurement relies on correct emission model and precise distance to source
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X7
X5
47 Tucanae(NGC 104)
Chandra ACIS-S0.38 keV
Heinke et al. ApJ, 625, 796 (2005) Bogdanov et al. ApJ, 646, 1104 (2006)
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NGC 6397
Chandra ACIS-S0.36 keV Bogdanov et al. ApJ, 709, 241 (2010)
U24
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M28 (NGC 6626)
Bogdanov et al. ApJ, 730, 81 (2011)Servillat et al. MNRAS, 453, 1556 (2012)
26
Chandra ACIS–S0.3–6 keV
237 ks
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Terzan 5Chandra ACIS–S
0.5–6 keV
710 ks
Bahramian et al. in prep.
Bogdanov et al. in prep.
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Photon energy (keV)
Spectroscopy of quiescent low-mass X-ray binaries
Bogdanov, Heinke, Özel, Güver, ApJ, 831, 184 (2016)
Chandra ACIS-S 1/8 subarray (200 ks)
1 10
• NS M-R estimates from an ensemble of systems can provide stringent constraints on the dense matter EoS
pileup not modeledpileup modeled
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Neutron Star Mass-Radius Constraints with Lynx
Photon energy (keV)
Chandra ACIS-S 1/8 subarray (200 ks)
1 10
Lynxmicro-calorimeter (200 ks)
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A complete census of rotation-powered MSPs
in globular clusters
Blind X-ray timing searches could discover all MSPs in nearby clusters
Bogdanov, Grindlay, & Rybicki, ApJ, 689, 407 (2008)
Bogdanov et al. ApJ, 646, 1104 (2006)
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Transitional Pulsars
Rotation-powered (radio) MSPs Accretion-powered (X-ray) MSPs
Papitto et al. Nature, 501, 517 (2013)
Chandra HRC IGR J182452452
Bogdanov et al. ApJ, 789, 40 (2014)
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X9
47 Tucanae(NGC 104)
Chandra ACIS-S0.38 keV
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47 Tuc X9: An Ultracompact Black Hole X-ray Binary
contemporaneous Chandra + NuSTAR + ATCA observations
• A 28 minute binary with a C-O WD donor and BH accretor!
Bahramian et al. MNRAS, 467, 2199 (2017)
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Conclusions
• Lynx observations of NS qLMXBs in globular clusters can produce stringent dense matter EoS constraints
• Bonus science from the same observations: cataclysmic variables, chromospherically active binaries, radio millisecond pulsars, transitional pulsars, black hole LMXBs, etc.
• Sub-arcsecond angular resolution is essential!
Einstein ROSAT Chandra
Pooley, PNAS, 107, 7164 (2010)
47 Tuc