Possible Time Correlation Between Jet Ejection and Mass Accretion for RW Aur A

• DOI: 10.48550/arxiv.2007.15848
• Publication Date: 2020-01-01
• Authors: M. Takami; Tracy L. Beck; P. C. Schneider; Hans Moritz Guenther; Marc White; K. N. Grankin; Jennifer L. Karr; Youichi Ohyama; Deirdre Coffey; Hauyu Baobab Liu; Roberto Galván-Ma...; Chun‐Fan Liu; Misato Fukagawa; N. Manset; Wen-Ping Chen; Tae‐Soo Pyo; Hsien Shang; T. P. Ray; Masaaki Otsuka; Mei-Yin Chou
• Keywords: Astrophysics - Solar and Stellar Astrophysics; 13. Climate action; 0103 physical sciences; FOS: Physical sciences; 01 natural sciences; Solar and Stellar Astrophysics (astro-ph.SR)

For the active T-Taur star RW Aur A we have performed long-term (~10 yr) monitoring observations of (1) jet imaging in [Fe II] 1.644-micron emission line using Gemini-NIFS and VLT-SINFONI; (2) optical high-resolution spectroscopy CFHT-ESPaDOnS; (3) V-band photometry CrAO 1.25-m telescope AAVSO. The latter two confirm correlation time variabilities between (A) Ca II 8542 O I 7772 profiles associated with magnetospheric accretion, (B) continuum fluxes. images their proper motions show that four knot ejections occurred at over past ~15 years an irregular interval 2-6 years. scale irregularity these intervals are similar to those dimming events seen data. Our a possible link remarkable (Delta_V < -1 mag.) photometric rises ejections. Observations another few may or reject this trend. If confirmed, would imply location launching region is very close (r <<0.1 au) as predicted by some models. Such conclusion be crucial for understanding disk evolution within au star, therefore ongoing planet formation radii.