We propose to study the weak coronae of flat activity stars - objects withvery low, nearly constant chromospheric emission. There is evidence that in manycases, these coronae are powered by magnetic fields from the residual turbulentdynamo left while the star.s cyclic dynamo is in a temporary Maunder-likemagnetic minimum. These stars permit us to 1) study the weakest and likely leastcomplex coronae, 2) investigate the coronal product of a turbulent dynamo in asolar mass star, and 3) explore (by proxy) the properties of the solar corona ina Maunder-like minimum.
Publications
The XMM-Newton serendipitous survey. V. The Second XMM-Newton serendipitous source catalogue |Watson, M. G., Schroder, A. C., et al. | A&A | 493-339 | 2009 | 2009A&A...493..339W | http://ui.adsabs.harvard.edu/#abs/2009A&A...493..339W
Statistical evaluation of the flux cross-calibration of the XMM-Newton EPIC cameras |Mateos, S., Saxton, R. D., et al. | A&A | 496-879 | 2009 | 2009A&A...496..879M | http://ui.adsabs.harvard.edu/#abs/2009A&A...496..879M
The XMM Cluster Survey: optical analysis methodology and the first data release |Mehrtens, Nicola, Romer, A. Kathy, et al. | MNRAS | 423-1024 | 2012 | 2012MNRAS.423.1024M | http://ui.adsabs.harvard.edu/#abs/2012MNRAS.423.1024M
Sunyaev-Zel.dovich effect or not? Detecting the main foreground effect of most galaxy clusters |Xiao, Weike, Chen, Chen, et al. | MNRAS | 432-41 | 2013 | 2013MNRAS.432L..41X | http://ui.adsabs.harvard.edu/#abs/2013MNRAS.432L..41X
Chandra Follow-up of the SDSS DR8 Redmapper Catalog Using the MATCha Pipeline |Hollowood, Devon L., Jeltema, Tesla, et al. | ApJS | 244-22 | 2019 | 2019ApJS..244...22H | http://ui.adsabs.harvard.edu/#abs/2019ApJS..244...22H
Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters |Palmese, A., Annis, J., et al. | MNRAS | 493-4591 | 2020 | 2020MNRAS.493.4591P | http://ui.adsabs.harvard.edu/#abs/2020MNRAS.493.4591P
The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII, O VIII, and Fe L-shell Transitions |Pan, Zeyang, Qu, Zhijie, et al. | ApJS | 271-62 | 2024 | 2024ApJS..271...62P | http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P
Robust constraints on feebly interacting particles using XMM-Newton |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-L101305 | 2024 | 2024PhRvD.109j1305L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L
Multimessenger search for electrophilic feebly interacting particles from supernovae |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-103028 | 2024 | 2024PhRvD.109j3028L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L
Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints |De la Torre Luque, Pedro, Balaji, Shyam, | ApJ | 968-46 | 2024 | 2024ApJ...968...46D | http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2004-01-22T21:54:48Z/2004-01-23T15:35:02Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
European Space Agency, Dr STEVEN SAAR, 2005, 'THE CORONAE OF EXTREMELY INACTIVE openParMAUNDER MINIMUMquestionMarkclosePar STARS', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-6mb3f06
