%0 Journal Article %1 citeulike:13096060 %A Aarnio, Alicia %A Stassun, Keivan %A Matt, Sean %D 2014 %J Proceedings of the International Astronomical Union %K imported %N S300 %P 318--321 %R 10.1017/s1743921313011149 %T Coronal Mass Ejections and Angular Momentum Loss in Young Stars %U http://dx.doi.org/10.1017/s1743921313011149 %V 8 %X In our own solar system, the necessity of understanding space weather is readily evident. Fortunately for Earth, our nearest stellar neighbor is relatively quiet, exhibiting activity levels several orders of magnitude lower than young, solar-type stars. In protoplanetary systems, stellar magnetic phenomena observed are analogous to the solar case, but dramatically enhanced on all physical scales: bigger, more energetic, more frequent. While coronal mass ejections (CMEs) could play a signi?cant role in the evolution of protoplanets, they could also a?ffect the evolution of the central star itself. To assess the consequences of prominence eruption/CMEs, we have invoked the solar-stellar connection to estimate, for young, solar-type stars, how frequently stellar CMEs may occur and their attendant mass and angular momentum loss rates. We will demonstrate the necessary conditions under which CMEs could slow stellar rotation.

@article{citeulike:13096060, abstract = {{In our own solar system, the necessity of understanding space weather is readily evident. Fortunately for Earth, our nearest stellar neighbor is relatively quiet, exhibiting activity levels several orders of magnitude lower than young, solar-type stars. In protoplanetary systems, stellar magnetic phenomena observed are analogous to the solar case, but dramatically enhanced on all physical scales: bigger, more energetic, more frequent. While coronal mass ejections (CMEs) could play a signi?cant role in the evolution of protoplanets, they could also a?ffect the evolution of the central star itself. To assess the consequences of prominence eruption/CMEs, we have invoked the solar-stellar connection to estimate, for young, solar-type stars, how frequently stellar CMEs may occur and their attendant mass and angular momentum loss rates. We will demonstrate the necessary conditions under which CMEs could slow stellar rotation.}}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Aarnio, Alicia and Stassun, Keivan and Matt, Sean}, biburl = {https://www.bibsonomy.org/bibtex/203d6d0548f9a2f959efd9eabd764a26d/ericblackman}, citeulike-article-id = {13096060}, citeulike-linkout-0 = {http://arxiv.org/abs/1403.0006}, citeulike-linkout-1 = {http://arxiv.org/pdf/1403.0006}, citeulike-linkout-2 = {http://dx.doi.org/10.1017/s1743921313011149}, day = 28, doi = {10.1017/s1743921313011149}, eprint = {1403.0006}, interhash = {b5d2d701bc6b8a45f3d5434d31ae4cbf}, intrahash = {03d6d0548f9a2f959efd9eabd764a26d}, issn = {1743-9213}, journal = {Proceedings of the International Astronomical Union}, keywords = {imported}, month = feb, number = {S300}, pages = {318--321}, posted-at = {2014-03-07 04:22:19}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{Coronal Mass Ejections and Angular Momentum Loss in Young Stars}}, url = {http://dx.doi.org/10.1017/s1743921313011149}, volume = 8, year = 2014 }