Typed states for the displayed outbound observations.
Source: paper_references, paper_reference_links
Paper Citation Record · LEDGER
Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
As of 17 August 2026, this Paper Citation Record lists 0 of 0 outbound references and 7 inbound Pith citation observations for arXiv:1701.08618.
A citation records a reference. It does not transfer a finding from one paper to another.
Coverage vector
One-hop event checks from named stored sources.
Source: scholarly_work_events, retraction_status_cache, observed 2026-08-17T06:30:58.91139+00:00
Pith citing papers itemized under the disclosed page cap.
Source: paper_references, paper_reference_links, observed 2026-08-15T14:41:13.631450Z
A source-named dated measurement, never combined with another source.
Source: pith, observed 2026-08-05T11:20:43.734257Z
Reference resolution
0 of 0 outbound references displayed
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External citation measurements
No source-named external measurement is stored.
Outbound references
No outbound reference observations are available for this paper version.
Pith citing papers
Observation 591a3658-2202-47c4-a7f8-b20b32e764fb · inbound
Probing clumpy wind accretion in IGR J18027-2016 with XMM-Newton cites this paper.
Probing clumpy wind accretion in IGR J18027-2016 with XMM-Newton Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 6
- Resolution
- unresolved
- no resolver link, observed 2026-08-14T14:12:15.841079Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.
Observation 32ae4616-6aa0-481e-b11b-74da9a86d735 · inbound
Cyclical accretion regime change in the slow X-ray pulsar 4U 0114+65 observed with Chandra cites this paper.
Cyclical accretion regime change in the slow X-ray pulsar 4U 0114+65 observed with Chandra Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 28
- Resolution
- unresolved
- no resolver link, observed 2026-08-10T20:26:26.106831Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.
Observation 393036e5-4feb-46d1-8069-17806563ab86 · inbound
Low-frequency observations of low-mass binary systems with neutron star candidates cites this paper.
Low-frequency observations of low-mass binary systems with neutron star candidates Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 40
- Resolution
- metadata mismatch
- local_arxiv, observed 2026-08-05T11:20:43.739083Z
Source-reported events for the cited work
No event found in the named queried sources as of 2026-08-17T06:30:58.91139+00:00.
Observation 706c0e51-f0fc-4ba2-a307-2c20951ece00 · inbound
The IACOB project XVIII. Prevalence of short-period binaries among Galactic helium rich O-type stars cites this paper.
The IACOB project XVIII. Prevalence of short-period binaries among Galactic helium rich O-type stars Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 139
- Resolution
- unresolved
- no resolver link, observed 2026-08-08T13:33:06.687563Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.
Observation c547d9a3-9ff8-4986-9634-b963b0b038dc · inbound
Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry cites this paper.
Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 139
- Resolution
- unresolved
- no resolver link, observed 2026-08-07T20:40:57.343717Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.
Observation bc6ede9f-63d3-418a-a34b-ea353ad781f4 · inbound
Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry cites this paper.
Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 139
- Resolution
- unresolved
- no resolver link, observed 2026-08-15T14:41:13.631450Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.
Observation fac06d06-424d-45ef-a0c5-1f678000643a · inbound
The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs cites this paper.
The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries
Reference 150
- Resolution
- unresolved
- no resolver link, observed 2026-08-14T15:20:02.651176Z
Source-reported events for the cited work
Unavailable: canonical work link unavailable.