pith. sign in

arxiv: 2606.26914 · v1 · pith:QXPDVW4Hnew · submitted 2026-06-25 · 🌌 astro-ph.HE

Transforming X-ray Binary Astrophysics with SKA+VLBI

Tao An , Ailing Wang , James C. A. Miller-Jones , Valeriu Tudose , Pikky Atri , Lang Cui , Hua Feng , Benito Marcote
show 1 more author
Sara E. Motta
This is my paper

Pith reviewed 2026-06-26 04:02 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords X-ray binariesVLBISKAjetsaccretionastrometrypolarimetryblack holes
0
0 comments X

The pith

The phased SKA-Mid as a VLBI element will transform radio studies of X-ray binaries via improved sensitivity, astrometry and rapid response.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper claims that running the SKA-Mid telescope in phased-array mode as one element in global VLBI networks will deliver substantially better radio data on X-ray binaries. The gains come from higher sensitivity on long baselines in key frequency bands, lower-frequency imaging with the connected array, microarcsecond position accuracy for bright sources, detailed polarization measurements, and fast response to new outbursts. A sympathetic reader would care because these features would let observers follow jet material on astronomical-unit scales, measure magnetic fields inside the jets, watch disk-jet coupling change in real time, and obtain accurate distances and birth kicks for the compact objects.

Core claim

The phased SKA-Mid operating as a single ultra-sensitive VLBI element will transform radio studies of XRBs primarily through its time-domain capabilities: substantially improved sensitivity on VLBI baselines that include SKA-Mid in Bands 2 and 5, together with connected-element SKA-Mid imaging extending down to 0.35-1 GHz, microarcsecond-precision astrometry for bright systems, high-fidelity polarimetry for the most strongly polarized sources, and rapid target-of-opportunity response. In synergy with global VLBI networks, SKA+VLBI will track the evolution of compact ejecta and compact jets on AU scales, measure frequency-dependent core shifts to infer magnetic field strengths and gradients,

What carries the argument

The phased SKA-Mid functioning as an ultra-sensitive VLBI element in synergy with global VLBI networks, delivering time-domain high-resolution radio observations of XRBs.

If this is right

  • Track the evolution of compact ejecta and jets on astronomical-unit scales in the first days of outbursts.
  • Measure frequency-dependent core shifts to determine magnetic field strengths and gradients inside the jets.
  • Resolve disk-jet coupling during state transitions in real time with cadenced multi-frequency VLBI movies.
  • Determine precise distances and natal kicks for X-ray binaries through parallaxes and proper motions in an astrometric census.
  • Provide strictly simultaneous multi-band constraints on accretion-ejection physics and jet composition when combined with future X-ray and optical telescopes.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same microphysical jet measurements could be compared directly with observations of active galactic nuclei to test whether the same launching and propagation physics operate across eight orders of magnitude in black-hole mass.
  • An XRB astrometric census might uncover previously undetected natal kicks or orbital parameters that current lower-sensitivity arrays cannot reach.
  • Rapid ToO response combined with the outlined core-shift survey could capture rare, short-lived jet features whose magnetic-field evolution has never been mapped before.

Load-bearing premise

The SKA-Mid will be built and operated with the stated sensitivity, frequency bands, rapid target-of-opportunity response, and ability to operate as a phased VLBI element alongside existing global networks.

What would settle it

If SKA-Mid phased-array observations fail to produce measurable sensitivity gains on VLBI baselines to X-ray binaries or cannot deliver the expected microarcsecond astrometric precision, the claimed transformation would not occur.

Figures

Figures reproduced from arXiv: 2606.26914 by Ailing Wang, Benito Marcote, Hua Feng, James C. A. Miller-Jones, Lang Cui, Pikky Atri, Sara E. Motta, Tao An, Valeriu Tudose.

Figure 1
Figure 1. Figure 1: Benchmark for jet kinematics applied to Soft X-ray Transients (SXTs). Time-sequence radio images of GRS 1915+105 from 18 March to 16 April 1994 show the birth of compact knots from the core (cross) and their separation with apparent superluminal motion (𝛽app > 1); scale bar: 10,000 AU. Adapted from Mirabel and Rodríguez (1994). SKA-Mid phased for global VLBI will extend this kinematic diagnostic to faint, … view at source ↗
Figure 2
Figure 2. Figure 2: Fender–Belloni–Gallo schematic of X-ray binary state transitions and associated jet modes (Fender et al., 2004), annotated to illustrate the unique diagnostic power of SKA + VLBI. In the hard state, SKA+VLBI will resolve and astrometrically monitor the compact, self-absorbed core, enabling ejection timing measurements to timestamp jet launch relative to the X-ray spectral transition at AU scales. During th… view at source ↗
Figure 3
Figure 3. Figure 3: MeerKAT imaging has revealed a shell and hotspot system around Cygnus X-1, including a compact core and a ∼20 pc ring seen at 1.28 and 2.64 GHz (Atri et al., 2025). The shell (the U-shaped curve denoted by B2-B1-B3) and the substructures (B4, B5) within the shell are consistent with powerful jets impacting the interstellar medium (Gallo et al., 2005). Similar jet-inflated bubbles have recently been discove… view at source ↗
read the original abstract

X-ray binaries (XRBs) are unique laboratories where accretion, jets, strong gravity and magnetic fields can be probed on humanly tractable timescales. The phased SKA-Mid operating as a single, ultra-sensitive Very Long Baseline Interferometry (VLBI) element will transform radio studies of XRBs primarily through its time-domain capabilities: substantially improved sensitivity on VLBI baselines that include SKA-Mid in Bands 2 and 5, together with connected-element SKA-Mid imaging extending down to 0.35--1 GHz (Band 1), microarcsecond-precision astrometry for bright systems, high-fidelity polarimetry for the most strongly polarized sources, and rapid target-of-opportunity response. In synergy with global VLBI networks, SKA+VLBI will track the evolution of compact ejecta and compact jets on astronomical unit (AU) scales, measure frequency-dependent core shifts to infer magnetic field strengths and gradients, resolve disk--jet coupling during state transitions in real time, and determine precise distances and natal kicks via parallaxes and proper motions. Joint campaigns with future X-ray and optical telescopes will enable strictly simultaneous, multi-band constraints on accretion--ejection physics and on jet composition. We outline a quantitative program for \aastar\ and AA4, including cadenced, multi-frequency VLBI ``movies'' of jets over the first days of outbursts, an XRB astrometric census, and a core-shift survey, and we provide representative detection rates, magnetic field measurements and distance accuracies. These outcomes will set the microphysical foundation for jet physics across the mass scale from stellar-mass black holes and neutron stars to active galactic nuclei, and will establish SKA+VLBI as the definitive facility for time-domain, high-resolution XRB astrophysics.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 1 minor

Summary. The manuscript is a perspective paper projecting that the phased SKA-Mid, functioning as an ultra-sensitive VLBI element, will transform X-ray binary (XRB) studies via enhanced time-domain capabilities: improved sensitivity on VLBI baselines in Bands 2 and 5, connected-element imaging down to Band 1 (0.35-1 GHz), microarcsecond astrometry for bright sources, high-fidelity polarimetry, and rapid ToO response. In synergy with global VLBI networks, this will enable AU-scale tracking of ejecta and jets, frequency-dependent core-shift measurements to infer magnetic fields, real-time disk-jet coupling during state transitions, and precise parallaxes/proper motions for distances and natal kicks. The paper outlines a quantitative program for AA* and AA4 phases, including cadenced multi-frequency VLBI 'movies', an XRB astrometric census, and core-shift surveys, with representative detection rates, B-field measurements, and distance accuracies. These are framed as setting the microphysical foundation for jet physics across mass scales and establishing SKA+VLBI as the definitive high-resolution time-domain facility, with synergies for joint X-ray/optical campaigns.

Significance. If the stated SKA-Mid specifications are realized, the projections identify concrete pathways for resolving accretion-ejection physics on human timescales in XRBs and scaling those insights to AGN. The inclusion of quantitative estimates (detection rates, measurement precisions) makes the case more actionable and falsifiable against future operations. The emphasis on strictly simultaneous multi-band observations and the explicit linkage to jet composition and magnetic field gradients adds value by highlighting unique parameter space not accessible with current facilities.

minor comments (1)
  1. Abstract: the string "\aastar" is an unreplaced LaTeX command and should be rendered as "AA*" for readability.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive and constructive review. The assessment accurately captures the manuscript's focus on the time-domain capabilities of phased SKA-Mid as a VLBI element and the quantitative projections for XRB jet tracking, astrometry, and core-shift measurements. We are pleased with the recommendation to accept.

Circularity Check

0 steps flagged

No significant circularity

full rationale

This perspective paper contains no derivations, equations, fitted parameters, or quantitative predictions derived from internal data or models. All listed capabilities (sensitivity gains, astrometry, polarimetry, ToO response) are explicitly conditional on external instrument specifications for SKA-Mid that are stated as assumptions, not derived within the text. No self-citations, ansatzes, or uniqueness theorems are invoked to support any derivation chain. The content is forward-looking description of projected outcomes once the instrument parameters are granted; the derivation chain is empty by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The paper rests on external assumptions about SKA instrument performance and operational capabilities that are not derived or tested within the document.

pith-pipeline@v0.9.1-grok · 5886 in / 1112 out tokens · 42015 ms · 2026-06-26T04:02:53.149345+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

85 extracted references · 84 canonical work pages · 5 internal anchors

  1. [1]

    G.E.Andersonetal

    doi: 10.1093/mnras/stx898. G.E.Andersonetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/GemmaAnderson01. J. J. Andrews, K. Breivik, and S. Chatterjee.ApJ, 886(1):68, Nov

    work page doi:10.1093/mnras/stx898 2026

  2. [3]

    doi: 10.1093/mnras/stz2335. P. Atri et al.MNRAS, 493(1):L81–L86, Mar

    work page doi:10.1093/mnras/stz2335

  3. [4]

    doi: 10.1093/mnrasl/slaa010. P. Atri et al.A&A, 696:A223, Apr

    work page doi:10.1093/mnrasl/slaa010

  4. [5]

    doi: 10.1051/0004-6361/202452837. W. A. Baan and T. An.ApJ, 980(1):119, Feb

    work page doi:10.1051/0004-6361/202452837

  5. [6]

    doi: 10.3847/1538-4357/ada9ea. M. Bachetti et al.Nature, 514(7521):202–204, Oct

    work page doi:10.3847/1538-4357/ada9ea

  6. [7]

    doi: 10.1038/nature13791. T. M. Belloni, S. E. Motta, and T. Muñoz-Darias.Bulletin of the Astronomical Society of India, 39 (3):409–428, Sept

    work page doi:10.1038/nature13791

  7. [8]

    doi: 10.48550/arXiv.1109.3388. A. Beri et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1109.3388

  8. [9]

    , keywords =

    doi: 10.1086/157262. R.D.BlandfordandD.G.Payne.MNRAS,199:883–903,June1982.doi: 10.1093/mnras/199.4.883. R. D. Blandford and R. L. Znajek.MNRAS, 179:433–456, May

    work page doi:10.1086/157262

  9. [10]

    doi: 10.1093/mnras/179.3

    work page doi:10.1093/mnras/179.3

  10. [12]

    doi: 10.1038/s41550-020-1023-5. C. Brocksopp et al.MNRAS, 432(2):931–943, June

    work page doi:10.1038/s41550-020-1023-5

  11. [13]

    doi: 10.1093/mnras/stt493. A. Burrows, T. Wang, and D. Vartanyan.ApJ, 987(2):164, July

    work page doi:10.1093/mnras/stt493

  12. [14]

    doi: 10.3847/1538-4357/ addd04. P. Charlot et al.A&A, 644:A159, Dec

    work page doi:10.3847/1538-4357/

  13. [15]

    doi: 10.1051/0004-6361/202038368. H. Q. Cheng et al.ApJL, 991(2):L41, Oct

    work page doi:10.1051/0004-6361/202038368

  14. [16]

    doi: 10.3847/2041-8213/adf104. S. Corbel et al.ApJ, 632(1):504–513, Oct

    work page doi:10.3847/2041-8213/adf104 2041

  15. [17]

    doi: 10.1086/432499. S. Corbel et al.MNRAS, 421(4):2947–2955, Apr

    work page doi:10.1086/432499

  16. [18]

    doi: 10.1111/j.1365-2966.2012.20517.x. S. Corbel et al.MNRAS, 431:L107–L111, Apr

    work page doi:10.1111/j.1365-2966.2012.20517.x 2012

  17. [19]

    doi: 10.1093/mnrasl/slt018. M. Coriat et al.MNRAS, 414(1):677–690, June

    work page doi:10.1093/mnrasl/slt018

  18. [20]

    doi: 10.1111/j.1365-2966.2011.18433.x. D. Cseh et al.MNRAS, 439:L1–L5, Mar

    work page doi:10.1111/j.1365-2966.2011.18433.x 2011

  19. [21]

    doi: 10.1093/mnrasl/slt166. D. Cseh et al.MNRAS, 452(1):24–31, Sept

    work page doi:10.1093/mnrasl/slt166

  20. [22]

    doi: 10.1093/mnras/stv1308. L. Cui et al.ApJ, 983(2):147, Apr

    work page doi:10.1093/mnras/stv1308

  21. [23]

    doi: 10.3847/1538-4357/adc0f7. A. Della Croce et al.A&A, 690:A179, Oct

    work page doi:10.3847/1538-4357/adc0f7

  22. [24]

    doi: 10.1051/0004-6361/202450954. V. Dhawan, I. F. Mirabel, and L. F. Rodríguez.ApJ, 543(1):373–385, Nov

    work page doi:10.1051/0004-6361/202450954

  23. [25]

    doi: 10.1086/520111. C. Done, M. Gierliński, and A. Kubota.A&ARv, 15(1):1–66, Dec

    work page doi:10.1086/520111

  24. [26]

    doi: 10.1086/300537. E. Egron et al.ApJ, 906(1):10, Jan

    work page doi:10.1086/300537

  25. [27]

    doi: 10.3847/1538-4357/abc5b1. S. Fabrika.Astrophys. Space Phys. Rev., 12:1–152, Jan

    work page doi:10.3847/1538-4357/abc5b1

  26. [28]

    doi: 10.48550/arXiv.astro-ph/ 0603390. H. Falcke, E. Körding, and S. Markoff.A&A, 414:895–903, Feb

    work page doi:10.48550/arxiv.astro-ph/

  27. [29]

    doi: 10.1051/0004-6361: 20031683. R. Fender and T. Belloni.ARA&A, 42(1):317–364, Sept

    work page doi:10.1051/0004-6361:

  28. [30]

    053102.134031

    doi: 10.1146/annurev.astro.42. 053102.134031. R. Fender and E. Gallo.Space Sci. Rev., 183(1-4):323–337, Sept

    work page doi:10.1146/annurev.astro.42

  29. [31]

    doi: 10.1086/312128. R. P. Fender and S. E. Motta.Nature Astronomy, Sept

    work page doi:10.1086/312128

  30. [32]

    doi: 10.1038/s41550-025-02665-w. R. P. Fender et al.MNRAS, 336(1):39–46, Oct. 2002a. doi: 10.1046/j.1365-8711.2002.05701.x. R.P.Fenderetal.MNRAS,330(1):212–218,Feb.2002b. doi: 10.1046/j.1365-8711.2002.05072.x. R. P. Fender, T. M. Belloni, and E. Gallo.MNRAS, 355(4):1105–1118, Dec

    work page doi:10.1038/s41550-025-02665-w 2002

  31. [33]

    Computer Graphics Forum31(5), 1735–1744 (2012) https://doi.org/10.1111/j

    doi: 10.1111/j. 1365-2966.2004.08384.x. R.P.Fender,J.Homan,andT.M.Belloni.MNRAS,396(3):1370–1382,July2009. doi: 10.1111/j. 1365-2966.2009.14841.x. G. Fragione, A. Loeb, and F. A. Rasio.ApJL, 918(2):L38, Sept

    work page doi:10.1111/j 2004

  32. [34]

    doi: 10.3847/2041-8213/ ac225a. T. Fragos et al.ApJ, 697:1057–1070, June

    work page doi:10.3847/2041-8213/ 2041

  33. [35]

    doi: 10.1088/0004-637X/697/2/1057. C. L. Fryer.New Astron. Rev., 50(7-8):492–495, Oct

    work page doi:10.1088/0004-637x/697/2/1057

  34. [36]

    doi: 10.1016/j.newar.2006.06.052. E. Gallo, R. P. Fender, and G. G. Pooley.MNRAS, 344(1):60–72, Sept

    work page doi:10.1016/j.newar.2006.06.052 2006

  35. [38]

    doi: 10.1038/nature03879. S. Heinz.A&A, 388:L40–L43, June

    work page doi:10.1038/nature03879

  36. [39]

    doi: 10.1051/0004-6361:20020402. S. Heinz.MNRAS, 355(3):835–844, Dec

    work page doi:10.1051/0004-6361:20020402

  37. [40]

    doi: 10.1111/j.1365-2966.2004.08361.x. S. Heinz.ApJ, 636(1):316–322, Jan

    work page doi:10.1111/j.1365-2966.2004.08361.x 2004

  38. [41]

    doi: 10.1086/497954. S. Heinz and R. A. Sunyaev.MNRAS, 343(3):L59–L64, Aug

    work page doi:10.1086/497954

  39. [42]

    2003.06918.x

    doi: 10.1046/j.1365-8711. 2003.06918.x. R.M.HjellmingandM.P.Rupen.Nature,375(6531):464–468,June1995. doi: 10.1038/375464a0. G. Hobbs, D. R. Lorimer, A. G. Lyne, and M. Kramer.MNRAS, 360(3):974–992, July

    work page doi:10.1046/j.1365-8711 2003

  40. [43]

    doi: 10.1111/j.1365-2966.2005.09087.x. R. M. Jeffrey, K. M. Blundell, S. A. Trushkin, and A. J. Mioduszewski.MNRAS, 461(1):312–320, Sept

    work page doi:10.1111/j.1365-2966.2005.09087.x 2005

  41. [44]

    doi: 10.1093/mnras/stw1322. P. Kaaret, S. Corbel, A. H. Prestwich, and A. Zezas.Science, 299(5605):365–368, Jan

    work page doi:10.1093/mnras/stw1322

  42. [45]

    doi: 10.1126/science.1079610. P. Kaaret, H. Feng, and T. P. Roberts.ARA&A, 55(1):303–341, Aug

    work page doi:10.1126/science.1079610

  43. [46]

    doi: 10.1093/mnras/stw2002. L. Z. Kelley et al.ApJL, 725:L91–L96, Dec

    work page doi:10.1093/mnras/stw2002

  44. [47]

    E.Körding,H.Falcke,andS.Corbel.A&A,456(2):439–450,Sept.2006

    doi: 10.1088/2041-8205/725/1/L91. E.Körding,H.Falcke,andS.Corbel.A&A,456(2):439–450,Sept.2006. doi: 10.1051/0004-6361: 20054144. C. C. Lang, P. Kaaret, S. Corbel, and A. Mercer.ApJ, 666(1):79–85, Sept

    work page doi:10.1088/2041-8205/725/1/l91 2041

  45. [48]

    doi: 10.48550/arXiv.astro-ph/9712132. I. Mandel and B. Müller.MNRAS, 499(3):3214–3221, Dec

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9712132

  46. [49]

    doi: 10.1093/mnras/staa3043. B. Marcote et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1093/mnras/staa3043

  47. [50]

    doi: 10.1051/0004-6361/202556290. A. Marino et al.ApJL, 980(2):L36, Feb

    work page doi:10.1051/0004-6361/202556290

  48. [51]

    doi: 10.3847/2041-8213/ad9580. S. Markoff, H. Falcke, P. L. Biermann, and R. P. Fender. In M. M. Shapiro, T. Stanev, and J. P. Wefel, editors,Astrophysical Sources of High Energy Particles and Radiation, volume 44, page 135, Jan

    work page doi:10.3847/2041-8213/ad9580 2041

  49. [52]

    doi: 10.1086/497628

    S.Markoff,M.A.Nowak,andJ.Wilms.ApJ,635(2):1203–1216,Dec.2005. doi: 10.1086/497628. S. Markoff et al.ApJL, 812(2):L25, Oct

    work page doi:10.1086/497628 2005

  50. [53]

    doi: 10.1088/2041-8205/812/2/L25. I. Martí-Vidal, A. Roy, J. Conway, and A. J. Zensus.A&A, 587:A143, Mar

    work page doi:10.1088/2041-8205/812/2/l25 2041

  51. [55]

    1365-2966.2003.07017.x

    doi: 10.1046/j. 1365-2966.2003.07017.x. M. J. Middleton et al.Nature, 493(7431):187–190, Jan

    work page doi:10.1046/j 2003

  52. [56]

    doi: 10.1038/nature11697. J. C. A. Miller-Jones.PASA, 31:e016, Mar

    work page doi:10.1038/nature11697

  53. [57]

    doi: 10.1017/pasa.2014.7. J. C. A. Miller-Jones et al.MNRAS, 388(4):1751–1758, Aug

    work page doi:10.1017/pasa.2014.7 2014

  54. [58]

    2012.21704.x

    doi: 10.1111/j.1365-2966. 2008.13495.x. J. C. A. Miller-Jones et al.ApJL, 706(2):L230–L234, Dec

    work page doi:10.1111/j.1365-2966 2008

  55. [59]

    doi: 10.1088/0004-637X/706/2/ L230. J. C. A. Miller-Jones et al.MNRAS, 419(1):L49–L53, Jan

    work page doi:10.1088/0004-637x/706/2/

  56. [60]

    doi: 10.1111/j.1745-3933.2011. 01176.x. J. C. A. Miller-Jones et al.Nature, 569(7756):374–377, Apr

    work page doi:10.1111/j.1745-3933.2011 2011

  57. [61]

    doi: 10.1126/science. abb3363. I. F. Mirabel and L. F. Rodríguez.Nature, 371(6492):46–48, Sept

    work page doi:10.1126/science

  58. [62]

    I.F.MirabelandL.F.Rodríguez.ARA&A,37:409–443, Jan.1999

    doi: 10.1038/371046a0. I.F.MirabelandL.F.Rodríguez.ARA&A,37:409–443, Jan.1999. doi: 10.1146/annurev.astro.37. 1.409. I. F. Mirabel et al.Nature, 413(6852):139–141, Sept

    work page doi:10.1038/371046a0 1999

  59. [63]

    doi: 10.1038/35093060. S. E. Motta et al.A&A, 696:A222, Apr

    work page doi:10.1038/35093060

  60. [64]

    21 Transforming XRB Astrophysics with SKA+VLBI T

    doi: 10.1051/0004-6361/202452838. 21 Transforming XRB Astrophysics with SKA+VLBI T. An et al. P.NagarajanandK.El-Badry.PASP,137(3):034203,Mar.2025. doi: 10.1088/1538-3873/adb6d6. S. Naoz, Z. Haiman, E. Quataert, and L. Holzknecht.ApJL, 992(1):L12, Oct

    work page doi:10.1051/0004-6361/202452838 2025

  61. [65]

    doi: 10.3847/ 2041-8213/ae0a20. T. N. O’Doherty et al.MNRAS, 521(2):2504–2524, May

    2041

  62. [66]

    doi: 10.1093/mnras/stad680. M. W. Pakull, R. Soria, and C. Motch.Nature, 466(7303):209–212, July

    work page doi:10.1093/mnras/stad680

  63. [67]

    doi: 10.48550/arXiv.astro-ph/9907169. Z. Paragi et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 143, Apr

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9907169

  64. [68]

    doi: 10.22323/1.215.0143. M. Pathak et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.22323/1.215.0143

  65. [69]

    doi: 10.1093/mnras/stab644. J. Poutanen et al.Science, 375(6583):874–876, Feb

    work page doi:10.1093/mnras/stab644

  66. [70]

    doi: 10.1126/science.abl4679. S. Prabu et al.MNRAS, 525(3):4426–4436, Nov

    work page doi:10.1126/science.abl4679

  67. [71]

    doi: 10.1093/mnras/stad2570. M. J. Reid et al.ApJ, 742(2):83, Dec

    work page doi:10.1093/mnras/stad2570

  68. [72]

    doi: 10.1088/0004-637X/742/2/83. R. A. Remillard and J. E. McClintock.ARA&A, 44(1):49–92, Sept

    work page doi:10.1088/0004-637x/742/2/83

  69. [73]

    Broadband reflection spectroscopy of MAXI J1535-571 using AstroSat: Estimation of black hole mass and spin

    doi: 10.1146/annurev. astro.44.051905.092532. M.Riojaetal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Rioja01. M. J. Rioja et al.AJ, 153(3):105, Mar

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev 2026

  70. [74]

    D.M.RussellandT.Shahbaz.MNRAS,438(3):2083–2096,Mar.2014.doi: 10.1093/mnras/stt2330

    doi: 10.3847/1538-3881/153/3/105. D.M.RussellandT.Shahbaz.MNRAS,438(3):2083–2096,Mar.2014.doi: 10.1093/mnras/stt2330. D. M. Russell, R. P. Fender, E. Gallo, and C. R. Kaiser.MNRAS, 376(3):1341–1349, Apr

    work page doi:10.3847/1538-3881/153/3/105 2083

  71. [75]

    doi: 10.1111/j.1365-2966.2007.11539.x. T. D. Russell et al.MNRAS, 439(2):1390–1402, Apr

    work page doi:10.1111/j.1365-2966.2007.11539.x 2007

  72. [76]

    doi: 10.1093/mnras/stt2498. T. D. Russell et al.ApJ, 883(2):198, Oct

    work page doi:10.1093/mnras/stt2498

  73. [77]

    doi: 10.3847/1538-4357/ab3d36. R. Sharma, M. Massi, and G. Torricelli-Ciamponi.A&A, 660:A58, Apr

    work page doi:10.3847/1538-4357/ab3d36

  74. [78]

    doi: 10.1093/mnrasl/sls044. K. V. Sokolovsky, Y. Y. Kovalev, A. B. Pushkarev, and A. P. Lobanov.A&A, 532:A38, Aug

    work page doi:10.1093/mnrasl/sls044

  75. [79]

    doi: 10.1051/0004-6361/201016072. R. Soria et al.MNRAS, 409(2):541–551, Dec

    work page doi:10.1051/0004-6361/201016072

  76. [80]

    doi: 10.1111/j.1365-2966.2010.17360.x. T. Sukhbold et al.ApJ, 821(1):38, Apr

    work page doi:10.1111/j.1365-2966.2010.17360.x 2010

  77. [81]

    doi: 10.3847/0004-637X/821/1/38. A. Tchekhovskoy, R. Narayan, and J. C. McKinney.MNRAS, 418(1):L79–L83, Nov

    work page internal anchor Pith review doi:10.3847/0004-637x/821/1/38

  78. [82]

    doi: 10.1111/j.1745-3933.2011.01147.x. S. J. Tingay et al.Nature, 374(6518):141–143, Mar

    work page doi:10.1111/j.1745-3933.2011.01147.x 2011

  79. [83]

    doi: 10.1038/374141a0. V. Tudose et al.MNRAS, 375(1):L11–L15, Feb

    work page doi:10.1038/374141a0

  80. [84]

    doi: 10.1111/j.1745-3933.2006.00264.x. F. Verbunt, A. Igoshev, and E. Cator.A&A, 608:A57, Dec

    work page doi:10.1111/j.1745-3933.2006.00264.x 2006

Showing first 80 references.