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The More The Merrier: Multi-Messenger Science with Gravitational Waves

Explore the various aspects of gravitational wave science, including EOS constraints using Binary NS Mergers, GW sources for LIGO and Virgo, progenitors of GRBs and kilonovae, and more.

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The More The Merrier: Multi-Messenger Science with Gravitational Waves

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  1. The More The Merrier: Multi-Messenger Science with Gravitational Waves Xiamen-CUSTIPEN Workshop, Xiamen January 4th 2019 [with focus on EOS constraints using Binary NS Mergers]

  2. LIGO + (2017) • or Why study them? • GW sources for LIGO, Virgo, … • progenitors of GRBs, kilonovae • r-process nucleosynthesis • constraining EOS(LIGO17, …) • ‘standard sirens’ / H0(Schutz86, LIGO17, Guidorzi+17) • tests of GR, e.g. speed of gravitational waves (LIGO17) • binary stellar evolution, NS formation channels • Binary NS Merger Science: multi-messenger

  3. LIGO + (2017) • or Why study them? • GW sources for LIGO, Virgo, … • progenitors of GRBs, kilonovae • r-process nucleosynthesis • constraining EOS(LIGO17, …) • ‘standard sirens’ / H0(Schutz86, LIGO17, Guidorzi+17) • tests of GR, e.g. speed of gravitational waves (LIGO17) • binary stellar evolution, NS formation channels • Binary NS Merger Science: multi-messenger

  4. Merger Remnant: schematics of a merger: • dependent on binary mass • dependent on EOS GW loss timescale inspiral merger

  5. Merger Remnant: GW loss timescale inspiral merger (see also Bartos+13)

  6. Merger Remnant: reminder: = maximum mass of cold, non-rotating NS where GW loss timescale inspiral merger (see also Bartos+13)

  7. Merger Remnant: GW loss timescale inspiral merger (see also Bartos+13)

  8. Merger Remnant: dynamical time prompt collapse GW loss timescale inspiral merger (see also Bartos+13)

  9. Merger Remnant: prompt collapse HMNS GW loss timescale dynamical time inspiral merger differential rotation (see also Bartos+13)

  10. Merger Remnant: prompt collapse HMNS GW loss timescale dynamical time SMNS viscous time inspiral merger differential rotation rigid rotation (see also Bartos+13)

  11. Merger Remnant: prompt collapse HMNS GW loss timescale dynamical time SMNS viscous time inspiral merger NS spin-down time differential rotation rigid rotation final remnant (see also Bartos+13)

  12. how to use to constrain NS EOS? • Multi-messenger EOS Constraints: prompt collapse HMNS dynamical time SMNS viscous time inspiral merger NS spin-down time differential rotation rigid rotation

  13. merger outcome • how to use to constrain NS EOS? • Multi-messenger EOS Constraints: prompt collapse HMNS dynamical time SMNS viscous time inspiral merger NS spin-down time differential rotation rigid rotation

  14. merger outcome • Multi-messenger EOS Constraints: • GW signal total binary mass,

  15. merger outcome • GW signal total binary mass, • Multi-messenger EOS Constraints: f(q) weakly dependent on q precisely measured less than 2% effect (for q>0.7)

  16. merger outcome • GW signal total binary mass, • Multi-messenger EOS Constraints: LIGO Virgo (2017) Time

  17. merger outcome • GW signal total binary mass, • Multi-messenger EOS Constraints: GW LIGO Virgo (2017) Time

  18. merger outcome • EM signature remnant fate(Bauswein+13; Metzger&Fernandez14; Metzger&Piro14; Kasen+15; …) • Multi-messenger EOS Constraints: GW

  19. merger outcome • EM signature remnant fate(Bauswein+13; Metzger&Fernandez14; Metzger&Piro14; Kasen+15; …) • Multi-messenger EOS Constraints: GW BM & Metzger (2017)

  20. merger outcome • EM signature remnant fate(Bauswein+13; Metzger&Fernandez14; Metzger&Piro14; Kasen+15; …) • Multi-messenger EOS Constraints: GW EM BM & Metzger (2017)

  21. merger outcome • EM signature remnant fate(Bauswein+13; Metzger&Fernandez14; Metzger&Piro14; Kasen+15; …) • Multi-messenger EOS Constraints: GW EOS EM BM & Metzger (2017)

  22. Application to GW170817: (I) remnant fate LIGO + (2017)

  23. Application to GW170817: (I) remnant fate prompt collapse HMNS dynamical time SMNS viscous time inspiral merger NS spin-down time differential rotation rigid rotation

  24. rule out long-lived SMNS or stable NS remnant • main argument: energetics • Application to GW170817: (I) remnant fate prompt collapse HMNS dynamical time SMNS viscous time inspiral merger NS spin-down time differential rotation rigid rotation for GW170817

  25. Application to GW170817: (II) energetics Radice+ (2018) baryonic mass angular momentum

  26. Application to GW170817: (II) energetics Radice+ (2018) merger remnant maximally rotating ! (Metzger,BM+15) baryonic mass angular momentum

  27. BM & Metzger (2017) • Application to GW170817: (II) energetics merger remnant maximally rotating ! rotational energy (erg) (Metzger,BM+15) remnant mass () (baryonic mass)

  28. BM & Metzger (2017) • Application to GW170817: (II) energetics ! (Metzger,BM+15) rotational energy (erg) remnant mass () (baryonic mass)

  29. BM & Metzger (2017) • Application to GW170817: (II) energetics ! • for stable remnant: tapped by magnetic-dipole spin-down () • inconsistent with GW170817 kilonova + afterglow(unless unusual ellipticity invoked) (Metzger,BM+15) rotational energy (erg) (Kiuchi+14, Metzger&Piro14, Siegel&Ciolfi16, …) remnant mass () (baryonic mass)

  30. BM & Metzger (2017) • Application to GW170817: (II) energetics ! • for stable remnant: tapped by magnetic-dipole spin-down () • inconsistent with GW170817 kilonova + afterglow(unless unusual ellipticity invoked) (Metzger,BM+15) GW170817 rotational energy (erg) (Kiuchi+14, Metzger&Piro14, Siegel&Ciolfi16, …) remnant mass () (baryonic mass)

  31. BM & Metzger (2017) • Application to GW170817: (II) energetics • rule out NS or SMNS remnant GW170817 rotational energy (erg) remnant mass () (baryonic mass)

  32. BM + (2018b) • Application to GW170817: (II) energetics • rule out NS or SMNS remnant • also strengthened by: • observed GRB post merger • lack of X-rays from NS spindown(BM+18b, Pooley+18) X-ray luminosity

  33. threshold masses EOS dependent • ruling out long-lived NS upper limit on • Application to GW170817: (III) constraints BH HMNS GW170817 SMNS NS

  34. threshold masses EOS dependent • ruling out long-lived NS upper limit on • Application to GW170817: (III) constraints BH HMNS GW170817 SMNS NS

  35. threshold masses EOS dependent • ruling out long-lived NS upper limit on • Application to GW170817: (III) constraints BH HMNS GW170817 SMNS NS

  36. BM & Metzger (2017) • find (BM&Metzger17) • Application to GW170817: (III) constraints NS radius (km) cumulative probability known NS masses (gravitational mass) NS maximal mass ()

  37. BM & Metzger (2017) • find (BM&Metzger17) • Application to GW170817: (III) constraints NS radius (km) cumulative probability known NS masses (gravitational mass) NS maximal mass ()

  38. BM & Metzger (2017) • find (BM&Metzger17) • relies only on qualitative categorization (HMNS / SMNS / …) • not sensitive to quantitative kilonova modeling uncertainties • Application to GW170817: (III) constraints NS radius (km) cumulative probability known NS masses (gravitational mass) NS maximal mass ()

  39. Coughlin, Dietrich, BM + (submitted) (but model dependent) • additional constraints from fitting kilonova ejecta properties • identify ejecta source (dynamical / disk winds) • ejecta mass & velocity depend on binary parameters and EOS • Additional Multi-Messenger Constraints: disk mass () 0.8 0.9 1.0 1.1 total mass / threshold mass for prompt collapse

  40. Coughlin, Dietrich, BM + (submitted) (but model dependent) • additional constraints from fitting kilonova ejecta properties • identify ejecta source (dynamical / disk winds) • ejecta mass & velocity depend on binary parameters and EOS • Additional Multi-Messenger Constraints: disk mass () EM 0.8 0.9 1.0 1.1 total mass / threshold mass for prompt collapse GW EOS:

  41. Bauswein + (2017) • Additional Multi-Messenger Constraints: • lack of prompt-collapse • from merger simulations: (Bauswein+13)+ causality: • (Bauswein+17) threshold for prompt-collapse increases with larger NS radius

  42. Future Outlook: • rich landscape (bright future)

  43. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future)

  44. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future) EOS learning opportunities

  45. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future) EOS learning opportunities

  46. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future) EOS learning opportunities

  47. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future) EOS learning opportunities & predictions!

  48. BM + (in prep) Multi-Messenger Matrix • Future Outlook: • rich landscape (bright future) EOS learning opportunities & predictions!

  49. prompt / HMNS NS / SMNS • Future Outlook: • for Galactic distribution of binary NSs(Kiziltan+13) ~32% BM + (in prep) ~3% EOS learning opportunities ~27% ~38% & predictions! SMNS HMNS / SMNS

  50. Ozel & Freire (2016) • Summary of EOS Constraints: • multi-messenger methods complementary to GW-only constraints (tidal deformability, post-merger signals, …) • future multi-messenger observations can further constrain EOS

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