1. MHD in weakly-ionised media Mark Wardle Macquarie University Sydney, Australia

2. Outline Molecular clouds and star formation MHD in weakly ionised media A comment on the hall effect Conductivity in molecular clouds Shock waves Conductivity in protostellar discs Implications for MRI and jets

3. Introduction

11. Magnetic fields in molecular clouds Magnetic fields play an important role during star formation –P mag is 30–100 times P gas in molecular clouds –energy density of magnetic field, fluid motions and self-gravity are similar –field removes angular momentum from cloud cores –field diffusion is required to avoid magnetic flux problem

13. MHD with finite conductivity

15. Conductivity

16. The Hall parameter relative strength of magnetic and drag forces in determining drift velocity particles tied to field particles tied to neutral fluid

17. For ions, For electrons,

18. The conductivity tensor solving for : current density: – field-parallel conductivity – Hall conductivity – Pedersen conductivity

19. Magnetic diffusion

20. If the only charged species are ions and electrons, Three distinct diffusion regimes: – Ohmic (resistive) – Hall – Ambipolar log n log B ohmic hall ambipolar

21. Hall effect in fully vs weakly ionised plasma Hall effect arises through asymmetry in tying of charged particles to magnetic field lines Fully ionised plasma: high frequencies, short wavelengths –difference between ion and electron cyclotron frequencies –ions can no longer keep up with changes to field –short lengthscales often irrelevant at the scales of interest –hall MHD etc Partially ionised plasma: low frequencies, long wavelengths –difference between ion and electron collision frequencies –neutral collisions decouple ions before electrons –length/time scale may be comparable to system size/evolutionary time scale –conductivity tensor in generalised Ohm’s law How does one reconcile these approaches? –in partially ionised case, ions become attached to the neutrals –effective ion mass is increased by ratio of neutral to ion densities –effective cyclotron frequency is reduced by same factor Be careful when estimating relevance of Hall effect!!!

23. Umebayashi & Nakano 1990

24. Nishi, Nakano & Umebayashi 1991

26. 0.1  m log  (10 15 cm kms -1 ) log n H (cm -3 )

27. MRN log  (10 15 cm kms -1 ) log n H (cm -3 )

28. log  (10 15 cm kms -1 ) log n H (cm -3 ) MRNi

29. log  (10 15 cm kms -1 ) log n H (cm -3 ) MRNx

30. J-type shock waves

32. C-type shock waves

35. Instability

37. Shock waves - Hall effect

38. Wardle 1998

40. Chapman & Wardle MNRAS in press

42. Stars, protostellar disks and planets

46. The minimum-mass solar nebula Simple model for surface density based on the solar system (Hayashi 1981) –add H,He etc to each planet to recover standard interstellar abundances –spread matter smoothly Resulting surface density: Disk mass: Useful reference standard

47. Temperature is estimated by considering thermal balance for a black solid particle –assume spherical, radius a, distance r from the sun: Then: – disk is thick beyond 30 AU – self-gravity negligible

58. Protostellar disks

59. Bachiller 1996 ARA&A

61. Kitamura et al 2002 ApJ

67. Protostellar disks Role of magnetic field in final stages of formation and subsequent evolution of protoplanetary discs is unclear –MHD turbulence (magnetorotational instability)? –disc-driven MHD winds? –disc corona? –dynamo activity? How strong is the magnetic field? Is the field coupled to the material in the disc? –disc is weakly ionised

68. Protostellar disks are poorly conducting high density implies low conductivity –recombinations relatively rapid –drag on charged particles deeper layers shielded from ionising radiation for r < 5 AU –x-ray attenuation column ~10 g/cm 2 –cosmic ray attenuation column ~100 g/cm 2

69. Igea & Glassgold 1999 cosmic rays x-ray ionisation rate

70. How strong is the magnetic field? Expect B > 10 mG given the strength in cloud cores Compression during formation of disk and star Shear in disc may wind up field or drive MRI Equipartition field in the minimum solar nebula Evidence for 0.1 – 1 G fields in the solar nebula at 1AU

71. Sano & Stone 2002a

72. Magnetic field diffusion in protostellar disks Is the magnetic field coupled to the matter? –  < h c s ? Which diffusion components dominate? –ohmic, hall or ambipolar? What are the consequences of different diffusion regimes? –vector evolution of B shows fundamental differences –hall diffusion reverses sign under global field reversal (yikes) Diffusion and magnetocentrifugal jet launching –loading of mass onto field lines –constrains bending of field lines within disk –radial drift of field Diffusivity depends on location –vertical stratification of ionisation rate and density –inconvenient radial variations of microphysics

73. Resistivity calculations minimum solar nebula –assume isothermal in z-direction ionisation by cosmic rays and x-rays from central star simple reaction scheme following Nishi, Nakano & Umebayashi (1993) –H +,H 3 +,He +,C +,molecular (M + ) and metal ions (M + ), e -, and charged grains –extended to allow high grain charge (T larger than in molecular clouds) adopt model for grains –none, single size grains, MRN size distribution, MRN+ice mantles, extended MRN, etc –results for “no grains” or 0.1  m grains presented here evaluate resistivity components –when can the field couple to the shear in the disc? –which form of diffusion is dominant?

74. Ionisation products

75. Reaction scheme

76. log n / n H  (s -1 ) M+M+ C+C+ m+m+ e He + H+H+ H3H3 + Abundances: 1AU, no grains z / h

77. Criterion for coupling

79. z / h log n / n H -14 0 1 2 3 -13  (s -1 ) -11 -12 M+M+ -4 -3 -2 C+C+ m+m+ e He + H+H+ H3H3 + Abundances: 1AU, 0.1  m grains

83. 5 AU

89. Magnetorotational instability (MRI) magnetic field couples different radii in disc tension transfers angular momentum outwards kh > 1 required to fit in disc, i.e. v A /c s < 1 resulting turbulence transports angular momentum outwards

90. MRI in non-ideal MHD Ambipolar or ohmic diffusion Hall diffusion Wardle 1999

91. Salmeron & Wardle 2005

93. Salmeron PhD thesis

94. Stone & Fleming 2003 MRI with dead zone

95. Sano & Stone 2002b MRI with hall diffusion

96. Sano & Stone 2002b log B 2 / 8πP 0

97. Protostellar jets

98. HH 30

99. Wardle 1997 IAU Coll. 163 (astro-ph)

100. Wardle 1997 IAU Coll. 163 (astro-ph)

101. Salmeron, Wardle & Königl