Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry | Paper Citation Record

Observation 76815f05-1d07-4971-bdcb-2cae2a165172 · outbound

This paper cites A persistent ultraviolet outflow from an accreting neutron star binary transient.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A persistent ultraviolet outflow from an accreting neutron star binary transient

Reference 1

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.812622Z

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Observation 1116b166-8e32-4446-89ea-7e7966d1d471 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 2

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.817542Z

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Observation b4a32427-05ae-4416-96a3-143ce58e0ea1 · outbound

This paper cites Soviet Physics Doklady , year = 1971, month = mar, volume =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Soviet Physics Doklady , year = 1971, month = mar, volume =

Reference 3

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.822261Z

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Observation f3362c8b-49fe-4c79-a43c-c682d6338dd3 · outbound

This paper cites On the absence of wind bow-shocks around OB-runaway stars: probing the physical conditions of the interstellar medium.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry On the absence of wind bow-shocks around OB-runaway stars: probing the physical conditions of the interstellar medium

Reference 4

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.826875Z

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Observation b4bf414d-6223-4821-966f-cd67094e581a · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 5

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.831288Z

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Observation 77d2b719-dd55-405a-9265-7cce8ee3d779 · outbound

This paper cites Quantifying jet-interstellar medium interactions in Cyg X-1: Insights from dual-frequency bow shock detection with MeerKAT.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Quantifying jet-interstellar medium interactions in Cyg X-1: Insights from dual-frequency bow shock detection with MeerKAT

Reference 6

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.835254Z

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Observation 5624112f-ccb8-42ae-8bb7-225708f82de9 · outbound

This paper cites , year = 1969, month = oct, volume =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , year = 1969, month = oct, volume =

Reference 7

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.839893Z

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Observation aad98ba4-3b27-4f13-9a47-047f41cfbb0a · outbound

This paper cites Gas Streams and Spiral Structure in the Milky Way.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Gas Streams and Spiral Structure in the Milky Way

Reference 8

Resolution: metadata mismatch; local_arxiv, observed 2026-08-07T20:40:58.627930Z

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No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation c343bbd1-4545-4369-a239-cec400c08f12 · outbound

This paper cites Blowing in the wind: The dust wave surrounding $\sigma$ Ori AB.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Blowing in the wind: The dust wave surrounding $\sigma$ Ori AB

Reference 9

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.848657Z

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Observation d770019b-9a1d-41c2-8719-6ed82a2de868 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 10

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.852739Z

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Observation aa594f6d-3a4f-478c-97c7-706272508d97 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 11

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.856552Z

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Observation bf347bf4-9e42-4000-9d64-b544275a3ba5 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 12

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.860377Z

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Observation 1cd1fc19-c8ea-4530-b2a5-cebe95cf5a66 · outbound

This paper cites Expansion Signatures in 35 HII Regions traced by SOFIA [CII] Emission.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Expansion Signatures in 35 HII Regions traced by SOFIA [CII] Emission

Reference 13

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.864151Z

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Observation 39792126-0776-4e8e-a6a9-5c9625ee376f · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 14

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.868142Z

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Observation 24856aba-da29-4d16-8a06-1e76feca385a · outbound

This paper cites Radiation-pressure-driven dust waves inside bursting interstellar bubbles.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Radiation-pressure-driven dust waves inside bursting interstellar bubbles

Reference 15

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.871993Z

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Observation 7ca1c674-18ab-4f40-a88b-783b64bc1773 · outbound

This paper cites ATLASGAL - Kinematic distances and the dense gas mass distribution of the inner Galaxy.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry ATLASGAL - Kinematic distances and the dense gas mass distribution of the inner Galaxy

Reference 16

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.875805Z

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Observation 86589a6a-7bb6-42a8-8623-7ccdcc853f2c · outbound

This paper cites Validation of the new Hipparcos reduction.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Validation of the new Hipparcos reduction

Reference 17

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.879551Z

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Observation cd674766-2fd6-4527-8423-f666d75912a4 · outbound

This paper cites Gaia Data Release 3: Summary of the content and survey properties.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Gaia Data Release 3: Summary of the content and survey properties

Reference 18

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.883395Z

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Observation 67bcf0af-85d3-4998-8303-73cba7cb47a6 · outbound

This paper cites X3: a high-mass Young Stellar Object close to the supermassive black hole Sgr~A*.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry X3: a high-mass Young Stellar Object close to the supermassive black hole Sgr~A*

Reference 19

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.887082Z

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Observation 87b43a56-153f-4ff1-9baa-af7a92585a11 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 20

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.581682Z

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No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation b6ecfcc5-f3c2-4abb-95fa-e05ce5d1d959 · outbound

This paper cites Interstellar Weather Vanes: GLIMPSE Mid-Infrared Stellar-Wind Bowshocks in M17 and RCW49.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Interstellar Weather Vanes: GLIMPSE Mid-Infrared Stellar-Wind Bowshocks in M17 and RCW49

Reference 21

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.894230Z

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Observation a1978628-fde8-4262-a47e-cfa13830b78e · outbound

This paper cites Cosmic ray acceleration and escape from supernova remnants.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Cosmic ray acceleration and escape from supernova remnants

Reference 22

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.897926Z

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Observation 82651d4f-666a-452b-b720-1505eb76532b · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 23

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.901510Z

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Observation a569e37b-9ab0-4ae9-bfef-3469e3f53c94 · outbound

This paper cites Massive runaway stars in the Large Magellanic Cloud.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Massive runaway stars in the Large Magellanic Cloud

Reference 24

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.904744Z

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Observation ebd646d3-3fa3-4a18-93d8-3195253d1b85 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 25

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.908557Z

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Observation a816f4ba-6beb-4f95-a90f-ed6013e53f5f · outbound

This paper cites Massive runaway stars in the Small Magellanic Cloud.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Massive runaway stars in the Small Magellanic Cloud

Reference 26

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.912107Z

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Observation 5204e4e9-feea-4b6a-be8a-b3897d0e8a06 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 28

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.919901Z

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Observation 67b857b1-2879-46f0-a1f0-3537aee3ea37 · outbound

This paper cites OB runaway stars originating in the Vel OB1 association.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry OB runaway stars originating in the Vel OB1 association

Reference 29

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.923212Z

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Observation 59d194a7-c05b-4d8f-aa2c-cace8c3258cf · outbound

This paper cites A magnetic massive star has experienced a stellar merger.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A magnetic massive star has experienced a stellar merger

Reference 30

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.926708Z

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Observation 59004bd3-281f-41cf-a8f7-dd7d3357f111 · outbound

This paper cites Evolutionary status of the Of?p star HD148937 and of its surrounding nebula NGC6164/5.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Evolutionary status of the Of?p star HD148937 and of its surrounding nebula NGC6164/5

Reference 31

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.930612Z

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Observation 876135e0-1ff9-442d-b73b-1ab05cf672df · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 33

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.937886Z

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Observation 6ce1d5dc-30e1-4810-aeae-13537ac33bc9 · outbound

This paper cites Ultra-High-Energy Gamma-Ray Bubble around Microquasar V4641 Sgr.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Ultra-High-Energy Gamma-Ray Bubble around Microquasar V4641 Sgr

Reference 34

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.941783Z

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Observation a8656a00-afd0-444a-8a6b-4afebfd5b4a3 · outbound

This paper cites Observational constraints on stellar feedback in dwarf galaxies.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Observational constraints on stellar feedback in dwarf galaxies

Reference 36

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.949571Z

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Observation 3588ce2c-ba4d-444a-9218-68195de0038e · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 37

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.953627Z

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Observation 9d0750e5-db3c-4ab6-a305-a2e8eb96da7e · outbound

This paper cites Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars

Reference 38

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.957531Z

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Observation fd16109d-2fc1-4f27-830b-2e78299dc4e7 · outbound

This paper cites A dark jet dominates the power output of the stellar black hole Cygnus X-1.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A dark jet dominates the power output of the stellar black hole Cygnus X-1

Reference 39

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.961619Z

Source-reported events for the cited work

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Observation a4a125cc-ff4c-4e0c-98cb-1d63649d85ba · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 40

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.965863Z

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Observation 77e6d728-d9aa-4692-b9fc-9733fe5c8682 · outbound

This paper cites True versus apparent shapes of bow shocks.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry True versus apparent shapes of bow shocks

Reference 41

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.969567Z

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Observation a7d4629a-4912-4d4d-a397-9f212036d336 · outbound

This paper cites Modelling multi-wavelength observational characteristics of bow shocks from runaway early type stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Modelling multi-wavelength observational characteristics of bow shocks from runaway early type stars

Reference 42

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.973677Z

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Observation 3ed2f4f2-e1fb-4322-8327-f9dbe5c9a2e4 · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 43

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.562288Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation 2a4d3f5c-65de-410d-8a6a-aeeb2973d671 · outbound

This paper cites Self-similar champagne flows in HII regions.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Self-similar champagne flows in HII regions

Reference 44

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.981633Z

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Observation dc91a6de-a30b-4964-8851-ccc88fd001c7 · outbound

This paper cites The cometary HII regions of DR 21: Bow shocks or champagne flows or both?.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The cometary HII regions of DR 21: Bow shocks or champagne flows or both?

Reference 45

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.985487Z

Source-reported events for the cited work

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Observation 387d3ec5-1c7c-4d9c-a3d4-838c2c4cf5c6 · outbound

This paper cites The early evolution of young massive clusters. II. The kinematic history of NGC 6618 / M 17.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The early evolution of young massive clusters. II. The kinematic history of NGC 6618 / M 17

Reference 46

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.988794Z

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Observation d84158ee-682c-4a9a-9fae-2b43e57a3eef · outbound

This paper cites EWOCS-III: JWST observations of the supermassive star cluster Westerlund 1.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry EWOCS-III: JWST observations of the supermassive star cluster Westerlund 1

Reference 47

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.992281Z

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Observation b92204eb-163d-460a-a2c1-6d4ae7a91413 · outbound

This paper cites Bow shock sources close to the Galactic centre.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Bow shock sources close to the Galactic centre

Reference 48

Resolution: metadata mismatch; local_arxiv, observed 2026-08-07T20:40:58.550500Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation c1ce8ba8-097d-4c7a-b82a-501811741c19 · outbound

This paper cites Properties of bow-shock sources at the Galactic center.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Properties of bow-shock sources at the Galactic center

Reference 49

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:56.999352Z

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Observation 47a38d02-5fa0-4bc2-a166-c165eec4e76d · outbound

This paper cites Distribution and kinematics of atomic and molecular gas inside the Solar circle.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Distribution and kinematics of atomic and molecular gas inside the Solar circle

Reference 50

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.003202Z

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Observation 93d22988-4fb2-4b3b-9dec-934ebeb2613a · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 51

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.007074Z

Source-reported events for the cited work

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Observation f4719fec-efda-43ae-bf91-7c255ab1325e · outbound

This paper cites The Green Bank Telescope HII Region Discovery Survey: III. Kinematic Distances.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The Green Bank Telescope HII Region Discovery Survey: III. Kinematic Distances

Reference 52

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.010799Z

Source-reported events for the cited work

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Observation 6cb431b7-2f88-482e-8bde-552dd10887d3 · outbound

This paper cites Streaming Motions and Kinematic Distances to Molecular Clouds.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Streaming Motions and Kinematic Distances to Molecular Clouds

Reference 53

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.014722Z

Source-reported events for the cited work

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Observation 12451c07-a8be-4d57-9e18-80386f1ec962 · outbound

This paper cites Fundamental Parameters for Central Stars of 103 Infrared Bowshock Nebulae.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Fundamental Parameters for Central Stars of 103 Infrared Bowshock Nebulae

Reference 54

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.018568Z

Source-reported events for the cited work

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Observation 2c5dc56f-d668-43c7-99ab-85ea1c50b81a · outbound

This paper cites IR nebulae around bright massive stars as indicators for binary interactions.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry IR nebulae around bright massive stars as indicators for binary interactions

Reference 55

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.022481Z

Source-reported events for the cited work

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Observation e189bddc-693f-4ccf-98c1-bc16cc9340ad · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 56

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.026542Z

Source-reported events for the cited work

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Observation 529e50c4-4d97-4d1c-9e9a-4783bb555b5e · outbound

This paper cites MeerKAT discovers a jet-driven bow shock near GRS 1915+105. How an invisible large-scale jet sculpts a microquasar's environment.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry MeerKAT discovers a jet-driven bow shock near GRS 1915+105. How an invisible large-scale jet sculpts a microquasar's environment

Reference 57

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.031205Z

Source-reported events for the cited work

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Observation 7318eb3e-7552-41b6-bc9a-2b63c378eb87 · outbound

This paper cites Galactic runaway O and Be stars found using Gaia DR3.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Galactic runaway O and Be stars found using Gaia DR3

Reference 58

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.035282Z

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Observation fd811fea-1032-4c70-93af-0180ffc4fa52 · outbound

This paper cites Particle acceleration at the bow shock of runaway star LS 2355: non-thermal radio emission but no $\gamma$-ray counterpart.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Particle acceleration at the bow shock of runaway star LS 2355: non-thermal radio emission but no $\gamma$-ray counterpart

Reference 59

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.039228Z

Source-reported events for the cited work

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Observation d9eae649-b895-4d8f-a23e-d6a90b9083cd · outbound

This paper cites Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars

Reference 60

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.043382Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 8f4f5f5a-334a-4ad7-99e2-c491dc1c40e8 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 61

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.533961Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation 9fae2b97-b1db-4908-ae1d-a73003025517 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 62

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.051387Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 12d9b12c-9acf-4629-8e9c-3b9ed45a02c5 · outbound

This paper cites Bow shocks, bow waves, and dust waves. III. Diagnostics.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Bow shocks, bow waves, and dust waves. III. Diagnostics

Reference 63

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.055862Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 2f935896-90c2-43e7-a3b4-001486f83ebd · outbound

This paper cites Bow shocks, bow waves, and dust waves. II. Beyond the rip point.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Bow shocks, bow waves, and dust waves. II. Beyond the rip point

Reference 64

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.059981Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 726c8e6e-94ca-4c64-89bb-b3384f08bb30 · outbound

This paper cites Bow shocks, bow waves, and dust waves. I. Strong coupling limit.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Bow shocks, bow waves, and dust waves. I. Strong coupling limit

Reference 65

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.063902Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation dea0047d-c318-4f4d-b6fb-f2ddca927871 · outbound

This paper cites Modeling Nonaxisymmetric Bow Shocks: Solution Method and Exact Analytic Solutions.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Modeling Nonaxisymmetric Bow Shocks: Solution Method and Exact Analytic Solutions

Reference 66

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.067610Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 98a84f41-038e-4dc0-ab99-93af2770408f · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 67

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.071046Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 3f006cb5-d3ef-4174-824e-04fe8f3833c6 · outbound

This paper cites New stellar bow shocks and bubbles found around runaway stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry New stellar bow shocks and bubbles found around runaway stars

Reference 68

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.074330Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 3c746213-0336-494a-a129-e202fd813d4f · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 69

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.077778Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation b5dc519e-bb19-48f0-9e36-71daf21d20a7 · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 70

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.081139Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation bc7ecc81-b187-4046-9f49-ff78789a79a2 · outbound

This paper cites A very massive runaway star from Cygnus OB2.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A very massive runaway star from Cygnus OB2

Reference 71

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.084545Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 8149fdc5-9b07-483f-8f0b-068281a9ab27 · outbound

This paper cites The early evolution of young massive clusters: The kinematic history of NGC6611 / M16.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The early evolution of young massive clusters: The kinematic history of NGC6611 / M16

Reference 72

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.088428Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation ce0a0a11-4f15-4087-8ebd-5391d78d5aea · outbound

This paper cites Wind nebulae and supernova remnants of very massive stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Wind nebulae and supernova remnants of very massive stars

Reference 73

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.092342Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation b58b3300-ec88-4af8-aa3a-92c093e9bb2a · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 74

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.514046Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation 2d973fc2-b168-4c11-9c3b-f9dc6188bb16 · outbound

This paper cites Astropy: A Community Python Package for Astronomy.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Astropy: A Community Python Package for Astronomy

Reference 75

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.099737Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation dc76999b-8d2b-4e5d-870a-d6a07bb4515e · outbound

This paper cites The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Reference 76

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.103680Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 753bd21c-6201-4327-acb8-09a45c073ee1 · outbound

This paper cites emcee: The MCMC Hammer.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry emcee: The MCMC Hammer

Reference 77

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.107547Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation eb960de6-af75-452e-a0e6-2d459a5fac8d · outbound

This paper cites Harris and K.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Harris and K

Reference 78

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.111468Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 6aebce51-fe43-4802-bb09-8b4cabc5c766 · outbound

This paper cites Binary interaction dominates the evolution of massive stars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Binary interaction dominates the evolution of massive stars

Reference 79

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.115462Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 997baeb9-b9b5-438e-9c89-5579dd09db08 · outbound

This paper cites Radio emission from the high-mass X-ray binary BP Cru: first detection.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Radio emission from the high-mass X-ray binary BP Cru: first detection

Reference 80

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.119468Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 7154ff88-696f-4ca1-8057-179d0cecefc4 · outbound

This paper cites An XMM-Newton view of FeK{\alpha} in HMXBs.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry An XMM-Newton view of FeK{\alpha} in HMXBs

Reference 81

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.123430Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 6861a66a-b1ff-4dcb-8228-255b9dcc6e8b · outbound

This paper cites A Chandra survey of fluorescence Fe lines in X-ray Binaries at high resolution.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A Chandra survey of fluorescence Fe lines in X-ray Binaries at high resolution

Reference 82

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.127269Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 2ac3c2ba-19d1-435a-9217-d9a6415964b0 · outbound

This paper cites SFXTs versus classical SgXBs: Does the difference lie in the companion wind?.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry SFXTs versus classical SgXBs: Does the difference lie in the companion wind?

Reference 83

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.131224Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation df7384c7-a195-43e2-a2d5-0d885adc7263 · outbound

This paper cites Supergiant, fast, but not so transient 4U 1907+09.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Supergiant, fast, but not so transient 4U 1907+09

Reference 84

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.135077Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation d619a284-6ded-4940-903c-3ff53f00a420 · outbound

This paper cites The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

Reference 85

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.138936Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation fe8a84d8-fcce-4695-8a7a-14179cb9dc5d · outbound

This paper cites High proper motion X-ray binaries from the Yale Southern Proper Motion Survey.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry High proper motion X-ray binaries from the Yale Southern Proper Motion Survey

Reference 86

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.142809Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 9bb7c71c-7df3-4a8f-b901-d68b9ad540ff · outbound

This paper cites A Quick Look at the $3\,$GHz Radio Sky I. Source Statistics from the Very Large Array Sky Survey.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry A Quick Look at the $3\,$GHz Radio Sky I. Source Statistics from the Very Large Array Sky Survey

Reference 87

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.146732Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation c3ae6c91-e3e1-4c1f-b476-5a91c7f705a5 · outbound

This paper cites Coupling hydrodynamics with comoving frame radiative transfer: II. Stellar wind stratification in the high-mass X-ray binary Vela X-1.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Coupling hydrodynamics with comoving frame radiative transfer: II. Stellar wind stratification in the high-mass X-ray binary Vela X-1

Reference 88

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.150878Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 6c6d4e47-3760-454c-93df-4ad968ac7dde · outbound

This paper cites Revisiting the archetypical wind accretor Vela X-1 in depth -- A case study of a well-known X-ray binary and the limits of our knowledge.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Revisiting the archetypical wind accretor Vela X-1 in depth -- A case study of a well-known X-ray binary and the limits of our knowledge

Reference 89

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.154700Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 714152a4-3f4c-47f4-b2fd-d401a91d0b19 · outbound

This paper cites Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2

Reference 90

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.158368Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 53e47228-5fd2-450c-8b00-34ad997a745d · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 91

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.161689Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 267aa110-d913-4089-a1fa-5bc6a4c7b061 · outbound

This paper cites General-Relativistic Simulations of Four States of Accretion onto Millisecond Pulsars.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry General-Relativistic Simulations of Four States of Accretion onto Millisecond Pulsars

Reference 92

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.164845Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation b01aee57-3abe-472f-8148-7ec21491ee09 · outbound

This paper cites GRMHD Simulations of Accreting Neutron Stars with Non-Dipole Fields.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry GRMHD Simulations of Accreting Neutron Stars with Non-Dipole Fields

Reference 93

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.168256Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 47f068c1-1a94-47b9-be28-a17b08adafc1 · outbound

This paper cites , archivePrefix = "arXiv", eprint =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , archivePrefix = "arXiv", eprint =

Reference 94

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.171706Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation f9de2b4e-d1cf-4efd-b81f-f888f99d38b3 · outbound

This paper cites , archivePrefix = "arXiv", eprint =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , archivePrefix = "arXiv", eprint =

Reference 95

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.486581Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation 368c8165-8425-478d-b64b-dacee4fcff0d · outbound

This paper cites , archivePrefix = "arXiv", eprint =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , archivePrefix = "arXiv", eprint =

Reference 96

Resolution: verified exact; doi, observed 2026-08-07T20:40:58.474339Z

Source-reported events for the cited work

No event found in the named queried sources as of 2026-08-08T06:32:00.761636+00:00.

Observation fab3ac41-b076-420c-9e6f-58493f20a543 · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 97

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.183083Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 8f3cef64-2576-4302-bbad-d976e7a8e5cb · outbound

This paper cites The thermal-radiative wind in the neutron star low mass X-ray binary GX 13+1.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry The thermal-radiative wind in the neutron star low mass X-ray binary GX 13+1

Reference 98

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.186818Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation b58fc95e-5186-4a8b-b879-707fa532593c · outbound

This paper cites Thermal and radiation driving can produce observable disk winds in hard-state X-ray binaries.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Thermal and radiation driving can produce observable disk winds in hard-state X-ray binaries

Reference 99

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.190847Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation d041d051-6551-44ed-9993-ed4730a8930f · outbound

This paper cites , eprint =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , eprint =

Reference 100

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.194791Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 849278b2-e352-49e1-abe9-c62b9225e5c2 · outbound

This paper cites Disk reflection and a possible disk wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Disk reflection and a possible disk wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058

Reference 101

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.198424Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation f4a3996d-f172-4e08-bdf3-7e2822b662da · outbound

This paper cites an unresolved cited work.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry Unresolved cited work

Reference 102

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.202258Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

Observation 90532ec5-f4bc-4b0b-9fd6-0d167779a3fc · outbound

This paper cites , keywords =.

Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry , keywords =

Reference 103

Resolution: unresolved; no resolver link, observed 2026-08-07T20:40:57.206161Z

Source-reported events for the cited work

Unavailable: canonical work link unavailable.

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