It is that simple to use our free service. Give it a try! Enter a domain name or URL address in the form above and click the check button. Simply visit us, do a real-time website status check for the given web service and stay informed by bookmarking the results (in this case every time you visit the results page a new check will be performed and the status updated).

In short, if you are interrupted by an error message like server not found or connection timed out while you are browsing, the first thing you should check if it is just you or everyone else is noticing a service issue for that particular domain name. WHAT WE DO: Our online tool is one of the many services created to tell you when a website is experiencing trouble. Our results indicate that typical SNe IIn arise from progenitor stars that undergo luminous-blue-variable-like mass loss shortly before they, ,, We compile similar data for SNe IIn from the literature and discuss our results in the context of this larger sample. We measure the progenitor star wind velocities (600-1400 km s –1) for the SNe in our sample and derive pre-explosion mass-loss rates (0.026-0.12 M ☉ yr –1). Our light curves show a relatively long rise time (>20 days) followed by a slow decline stage (0.01-0.15 mag day –1), and a typical V-band peak magnitude of M V = –18.4 ± 1.0 mag. We find that a narrow P-Cygni profile in the hydrogen Balmer lines appears to be a ubiquitous feature of SNe IIn. Therefore, these events are representative of the observed population of SNe IIn. The CCCP SN sample is unbiased to the extent that object selection was not influenced by target SN properties. Here, we study the four SNe IIn observed by the Caltech Core-Collapse Project (CCCP). Type IIn supernovae (SNe IIn) are rare events, constituting only a few percent of all core-collapse SNe, and the current sample of well-observed SNe IIn is small.

Info on cccp project