Detail publikace

Fine-scale structure in cometary dust tails I: Analysis of striae in Comet C/2006 P1 (McNaught) through temporal mapping

PRICE, O. JONES, G. MORRILL, J. OWENS, M. BATTAMS, K. MORGAN, H. DRUCKMÜLLER, M. DEIRIES, S.

Anglický název

Fine-scale structure in cometary dust tails I: Analysis of striae in Comet C/2006 P1 (McNaught) through temporal mapping

Typ

článek v časopise ve Web of Science, Jimp

Jazyk

en

Originální abstrakt

Striated features, or striae, form in cometary dust tails due to an as-yet unconstrained process or processes. For the first time we directly display the formation of striae, at C/2006 P1 McNaught, using data from the SOHO LASCO C3 coronagraph. The nature of this formation suggests both fragmentation and shadowing effects are important in the formation process. Using the SOHO data with STEREO-A and B data from the HI-1 and HI-2 instruments, we display the evolution of these striae for two weeks, with a temporal resolution of two hours or better. This includes a period of morphological change on 2007 January 13-14 that we attribute to Lorentz forces caused by the comet's dust tail crossing the heliospheric current sheet. The nature of this interaction also implies a mixing of different sized dust along the striae, implying that fragmentation must be continuous or cascading. To enable this analysis, we have developed a new technique – temporal mapping – that displays cometary dust tails directly in the radiation beta (ratio of radiation pressure to gravity) and dust ejection time phase space. This allows for the combination of various data sets and the removal of transient motion and scaling effects.

Anglický abstrakt

Striated features, or striae, form in cometary dust tails due to an as-yet unconstrained process or processes. For the first time we directly display the formation of striae, at C/2006 P1 McNaught, using data from the SOHO LASCO C3 coronagraph. The nature of this formation suggests both fragmentation and shadowing effects are important in the formation process. Using the SOHO data with STEREO-A and B data from the HI-1 and HI-2 instruments, we display the evolution of these striae for two weeks, with a temporal resolution of two hours or better. This includes a period of morphological change on 2007 January 13-14 that we attribute to Lorentz forces caused by the comet's dust tail crossing the heliospheric current sheet. The nature of this interaction also implies a mixing of different sized dust along the striae, implying that fragmentation must be continuous or cascading. To enable this analysis, we have developed a new technique – temporal mapping – that displays cometary dust tails directly in the radiation beta (ratio of radiation pressure to gravity) and dust ejection time phase space. This allows for the combination of various data sets and the removal of transient motion and scaling effects.

Klíčová slova anglicky

Comets, Dust, Plasma, Solar wind

Vydáno

12.09.2018

Nakladatel

ACADEMIC PRESS INC ELSEVIER SCIENCE, 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA

Místo

SAN DIEGO, USA

ISSN

0019-1035

Ročník

319

Číslo

1

Strany od–do

540–557

Počet stran

18

BIBTEX


@article{BUT158953,
  author="Oliver {Price} and Geraint H. {Jones} and Jeff {Morrill} and Mathew {Owens} and Karl {Battams} and Huw {Morgan} and Miloslav {Druckmüller} and Sebastian {Deiries},
  title="Fine-scale structure in cometary dust tails I: Analysis of striae in Comet C/2006 P1 (McNaught) through temporal mapping",
  year="2018",
  volume="319",
  number="1",
  month="September",
  pages="540--557",
  publisher="ACADEMIC PRESS INC ELSEVIER SCIENCE, 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA",
  address="SAN DIEGO, USA",
  issn="0019-1035"
}